Joshua A Eisner

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Journals/Publications

• Otter, J., Ginsburg, A., Ballering, N. P., Bally, J., Eisner, J., Goddi, C., Plambeck, R., & Wright, M. (2021). "Small Protoplanetary Disks in the Orion Nebula Cluster and OMC1 with ALMA". apj, 923(2), 221.
• Sallum, S., Eisner, J., Stone, J., Dietrich, J., Hinz, P., & Spalding, E. (2021). "ELT Imaging of MWC 297 from the 23 m LBTI: Complex Disk Structure and a Companion Candidate". aj, 161(1), 28.
• Boyden, R. D., & Eisner, J. A. (2020). "Protoplanetary Disks in the Orion Nebula Cluster: Gas-disk Morphologies and Kinematics as Seen with ALMA". apj, 894(1), 74.
• Terwisga, S., Dishoeck, E., Mann, R., Di Francesco, J., Marel, N., Meyer, M., Andrews, S., Carpenter, J., Eisner, J., Manara, C., & Williams, J. (2020). "Protoplanetary disk masses in NGC 2024: Evidence for two populations". aap, 640, A27.
• Ballering, N. P., & Eisner, J. A. (2019). Erratum: textquotedblleftProtoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurustextquotedblright (2019, AJ, 157, 144). aj, 157(5), 214.
• Ballering, N. P., & Eisner, J. A. (2019). Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus. aj, 157(4), 144.
• Ballering, N., & Eisner, J. (2019). VizieR Online Data Catalog: Protoplanetary disk masses in Taurus (Ballering+, 2019). VizieR Online Data Catalog, J/AJ/157/144.
• Dong, R., Liu, S. -., Eisner, J., Andrews, S., Fung, J., Zhu, Z., Chiang, E., Hashimoto, J., Liu, H., Casassus, S., Esposito, T., Hasegawa, Y., Muto, T., Pavlyuchenkov, Y., Wilner, D., Akiyama, E., Tamura, M., & Wisniewski, J. (2019). VizieR Online Data Catalog: ALMA continuum emission obs. of MWC 758 disk (Dong+, 2018). VizieR Online Data Catalog, J/ApJ/860/124.
• Labdon, A., Kraus, S., Davies, C. L., Kreplin, A., Kluska, J., Harries, T. J., Monnier, J. D., Brummelaar, T., Baron, F., Millan-Gabet, R., Kloppenborg, B., Eisner, J., Sturmann, J., & Sturmann, L. (2019). Dusty disk winds at the sublimation rim of the highly inclined, low mass young stellar object SU Aurigae. aap, 627, A36.
• Sallum, S., Skemer, A., Eisner, J., Marel, N., Sheehan, P., Close, L., {Ireland, }. M., Males, J., Morzinski, K., Bailey, V., Briguglio, R., & Puglisi, A. (2019). New Spatially Resolved Imaging of the SR 21 Transition Disk and Constraints on the Small-grain Disk Geometry. apj, 883(1), 100.
• Sheehan, P. D., Wu, Y., Eisner, J. A., & Tobin, J. J. (2019). High-precision Dynamical Masses of Pre-main-sequence Stars with ALMA and Gaia. apj, 874(2), 136.
• Stone, J., Skemer, A., Hinz, P., Bonavita, M., Kratter, K., Maire, A. -., Defrere, D., Bailey, V., Spalding, E., Leisenring, J., Desidera, S., Bonnefoy, M., Biller, B., Woodward, C., Henning, T., Skrutskie, M., Eisner, J., Crepp, J., Patience, J., , Weigelt, G., et al. (2019). VizieR Online Data Catalog: The LEECH exoplanet imaging survey (Stone+, 2018). VizieR Online Data Catalog, J/AJ/156/286.
• Dong, R., Liu, S., Eisner, J., Andrews, S., Fung, J., Zhu, Z., Chiang, E., Hashimoto, J., Liu, H., Casassus, S., Esposito, T., Hasegawa, Y., Muto, T., Pavlyuchenkov, Y., Wilner, D., Akiyama, E., Tamura, M., & Wisniewski, J. (2018). The Eccentric Cavity, Triple Rings, Two-armed Spirals, and Double Clumps of the MWC 758 Disk. \apj, 860, 124.
• Eisner, J., Arce, H., Ballering, N., Bally, J., Andrews, S., Boyden, R., Di Francesco, J., Fang, M., Johnstone, D., Kim, J., Mann, R., Matthews, B., Pascucci, I., Ricci, L., Sheehan, P., & Williams, J. (2018). Protoplanetary Disk Properties in the Orion Nebula Cluster: Initial Results from Deep, High-resolution ALMA Observations. \apj, 860, 77.
• Sheehan, P., & Eisner, J. (2018). Multiple Gaps in the Disk of the Class I Protostar GY 91. \apj, 857, 18.
• Stone, J., Skemer, A., Hinz, P., Bonavita, M., Kratter, K., Maire, A., Defrere, D., Bailey, V., Spalding, E., Leisenring, J., Desidera, S., Bonnefoy, M., Biller, B., Woodward, C., Henning, T., Skrutskie, M., Eisner, J., Crepp, J., Patience, J., , Weigelt, G., et al. (2018). The LEECH Exoplanet Imaging Survey: Limits on Planet Occurrence Rates under Conservative Assumptions. \aj, 156, 286.
• Ballering, N., & Eisner, J. (2017). "Protoplanetary Disk Masses in Taurus and the Orion Nebula Cluster". LPI Contributions, 2042, 4133.
• Bally, J., Ginsburg, A., Arce, H., Eisner, J., Youngblood, A., Zapata, L., & Zinnecker, H. (2017). "The ALMA View of the OMC1 Explosion in Orion". apj, 837, 60.
• Kim, J., Pascucci, I., Allen, L., Apai, D., Bergin, T., Ciesla, F., Eisner, J., Fang, M., Krijt, S., Najita, J., Rieke, G., & Salyk, C. (2017). "Earths in Other Solar Systems: Fundamental Protoplanetary Disk Properties and Their Evolution". LPI Contributions, 2042, 4071.
• Sallum, S., & Eisner, J. (2017). "Data Reduction and Image Reconstruction Techniques for Non-redundant Masking". apjs, 233, 9.
• Sallum, S., Eisner, J., Hinz, P., Sheehan, P., Skemer, A., Tuthill, P., & Young, J. (2017). "Improved Constraints on the Disk around MWC 349A from the 23 m LBTI". apj, 844, 22.
• Sheehan, P., & Eisner, J. (2017). "Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud". apj, 851, 45.
• Sheehan, P., & Eisner, J. (2017). "WL 17: A Young Embedded Transition Disk". apjl, 840, L12.
• Wu, Y., Close, L., Eisner, J., & Sheehan, P. (2017). "An Explanation of the Very Low Radio Flux of Young Planet-mass Companions". aj, 154, 234.
• Armitage, P., Eisner, J., & Simon, J. (2016). "Prompt Planetesimal Formation beyond the Snow Line". apjl, 828, L2.
• Eisner, J., Bally, J., Ginsburg, A., & Sheehan, P. (2016). "Protoplanetary Disks in the Orion OMC1 Region Imaged with ALMA". apj, 826, 16.
• Eisner, J., Bally, J., Ginsburg, A., & Sheehan, P. (2016). "VizieR Online Data Catalog: ALMA and GeMS observations of the OMC1 region (Eisner+, 2016)". VizieR Online Data Catalog, 182.
• Schlieder, J., Skemer, A., Maire, A., Desidera, S., Hinz, P., Skrutskie, M., Leisenring, J., Bailey, V., Defr{`ere}, D., Esposito, S., Strassmeier, K., Weber, M., Biller, B., Bonnefoy, M., Buenzli, E., Close, L., Crepp, J., Eisner, J., Hofmann, K., , Henning, T., et al. (2016). "The LEECH Exoplanet Imaging Survey: Orbit and Component Masses of the Intermediate-Age, Late-Type Binary NO UMa". apj, 818, 1.
• Sheehan, P., Eisner, J., Mann, R., & Williams, J. (2016). "A VLA Survey for Faint Compact Radio Sources in the Orion Nebula Cluster". apj, 831, 155.
• Skemer, A., Morley, C., Zimmerman, N., Skrutskie, M., Leisenring, J., Buenzli, E., Bonnefoy, M., Bailey, V., Hinz, P., Defr{'ere}, D., Esposito, S., Apai, D., Biller, B., Brandner, W., Close, L., Crepp, J., De, R. R., Desidera, S., Eisner, J., , Fortney, J., et al. (2016). "The LEECH Exoplanet Imaging Survey: Characterization of the Coldest Directly Imaged Exoplanet, GJ 504 b, and Evidence for Superstellar Metallicity". apj, 817, 166.
• Stone, J., Eisner, J., Skemer, A., Morzinski, K., Close, L., Males, J., Rodigas, T., Hinz, P., & Puglisi, A. (2016). "L-band Spectroscopy with Magellan-AO/Clio2: First Results on Young Low-mass Companions". apj, 829, 39.
• Stone, J., Skemer, A., Kratter, K., Dupuy, T., Close, L., Eisner, J., Fortney, J., Hinz, P., Males, J., Morley, C., Morzinski, K., & Ward-Duong, K. .. (2016). "Adaptive Optics imaging of VHS 1256-1257: A Low Mass Companion to a Brown Dwarf Binary System". apjl, 818, L12.
• {Bally}, J., {Mann}, R., {Eisner}, J., {Andrews}, S., {Di Francesco}, J., {Hughes}, M., {Johnstone}, D., {Matthews}, B., {Ricci}, L., , J. (2015). "{ALMA Observations of the Largest Proto-Planetary Disk in the Orion Nebula, 114-426: A CO Silhouette}". apj, 808, 69.
• {Eisner}, J. (2015). "{Spectral Energy Distributions of Accreting Protoplanets}". apjl, 803, L4.
• {Eisner}, J., {Rieke}, G., {Rieke}, M., {Flaherty}, K., {Stone}, J., {Arnold}, T., {Cortes}, S., {Cox}, E., {Hawkins}, C., {Cole}, A., {Zajac}, S., , A. (2015). "{Time-monitoring observations of Br{$gamma$} emission from young stars}". mnras, 447, 202-217.
• {Hales}, A., {Corder}, S., {Dent}, W., {Andrews}, S., {Eisner}, J., , L. (2015). "{The Early ALMA View of the FU Ori Outburst System}". apj, 812, 134.
• {Maire}, A., {Skemer}, A., {Hinz}, P., {Desidera}, S., {Esposito}, S., {Gratton}, R., {Marzari}, F., {Skrutskie}, M., {Biller}, B., {Defr{`e}re}, D., {Bailey}, V., {Leisenring}, J., {Apai}, D., {Bonnefoy}, M., {Brandner}, W., {Buenzli}, E., {Claudi}, R., {Close}, L., {Crepp}, J., , {De Rosa}, R., et al. (2015). "{The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system (Corrigendum)}". aap, 579, C2.
• {Maire}, A., {Skemer}, A., {Hinz}, P., {Desidera}, S., {Esposito}, S., {Gratton}, R., {Marzari}, F., {Skrutskie}, M., {Biller}, B., {Defr{`e}re}, D., {Bailey}, V., {Leisenring}, J., {Apai}, D., {Bonnefoy}, M., {Brandner}, W., {Buenzli}, E., {Claudi}, R., {Close}, L., {Crepp}, J., , {De Rosa}, R., et al. (2015). "{The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system}". aap, 576, A133.
• {Mann}, R., {Andrews}, S., {Eisner}, J., {Williams}, J., {Meyer}, M., {Di Francesco}, J., {Carpenter}, J., , D. (2015). "{Protoplanetary Disk Masses in the Young NGC 2024 Cluster}". apj, 802, 77.
• {Miller}, A., {Bloom}, J., {Richards}, J., {Lee}, Y., {Starr}, D., {Butler}, N., {Tokarz}, S., {Smith}, N., , J. (2015). "{A Machine-learning Method to Infer Fundamental Stellar Parameters from Photometric Light Curves}". apj, 798, 122.
• {Sallum}, S., {Eisner}, J., {Close}, L., {Hinz}, P., {Skemer}, A., {Bailey}, V., {Briguglio}, R., {Follette}, K., {Males}, J., {Morzinski}, K., {Puglisi}, A., {Rodigas}, T., {Weinberger}, A., , M. (2015). "{New Spatially Resolved Observations of the T Cha Transition Disk and Constraints on the Previously Claimed Substellar Companion}". apj, 801, 85.
• {Sallum}, S., {Follette}, K., {Eisner}, J., {Close}, L., {Hinz}, P., {Kratter}, K., {Males}, J., {Skemer}, A., {Macintosh}, B., {Tuthill}, P., {Bailey}, V., {Defr{`e}re}, D., {Morzinski}, K., {Rodigas}, T., {Spalding}, E., {Vaz}, A., , A. (2015). "{Accreting protoplanets in the LkCa 15 transition disk}". nat, 527, 342-344.
• {Schlieder}, J., {Skemer}, A., {Maire}, A., {Desidera}, S., {Hinz}, P., {Skrutskie}, M., {Leisenring}, J., {Bailey}, V., {Defrere}, D., {Esposito}, S., {Strassmeier}, K., {Weber}, M., {Biller}, B., {Bonnefoy}, M., {Buenzli}, E., {Close}, L., {Crepp}, J., {Eisner}, J., {Hofmann}, K., , {Henning}, T., et al. (2015). "{The LEECH Exoplanet Imaging Survey: Orbit and Component Masses of the Intermediate Age, Late-Type Binary NO UMa}". ArXiv e-prints.
• {Skemer}, A., {Morley}, C., {Zimmerman}, N., {Skrutskie}, M., {Leisenring}, J., {Buenzli}, E., {Bonnefoy}, M., {Bailey}, V., {Hinz}, P., {Defr{'e}re}, D., {Esposito}, S., {Apai}, D., {Biller}, B., {Brandner}, W., {Close}, L., {Crepp}, J., {De Rosa}, R., {Desidera}, S., {Eisner}, J., , {Fortney}, J., et al. (2015). "{The LEECH Exoplanet Imaging Survey: Characterization of the Coldest Directly Imaged Exoplanet, GJ 504 b, and Evidence for Super-Stellar Metallicity}". ArXiv e-prints.
• Eisner, J. A., Hillenbrand, L. A., & Stone, J. M. (2014). Constraining the sub-au-scale distribution of hydrogen and carbon monoxide gas around young stars with the Keck Interferometer. Monthly Notices of the Royal Astronomical Society, 443, 1916-1945.
• Sheehan, P. D., & Eisner, J. A. (2014). Constraining the Disk Masses of the Class I Binary Protostar GV Tau. Astrophysical Journal, 791, 19.
• Stone, J. M., Eisner, J. A., Salyk, C., Kulesa, C., & McCarthy, D. (2014). Variable Accretion Processes in the Young Binary-star System UY Aur. Astrophysical Journal, 792, 56.
• Woillez, J., Wizinowich, P., Akeson, R., Colavita, M., Eisner, J., Millan-Gabet, R., Monnier, J. D., Pott, J. -., & Ragland, S. (2014). First faint dual-field off-axis observations in optical long baseline interferometry. Astrophysical Journal, 783(2).
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  Abstract: Ground-based long baseline interferometers have long been limited in sensitivity in part by the short integration periods imposed by atmospheric turbulence. The first observation fainter than this limit was performed on 2011 January 22 when the Keck Interferometer observed a K = 11.5 target, about 1 mag fainter than its K = 10.3 atmospherically imposed limit; the currently demonstrated limit is K = 12.5. These observations were made possible by the Dual-Field Phase-Referencing (DFPR) instrument, part of the NSF-funded ASTrometry and phase-Referenced Astronomy project; integration times longer than the turbulence time scale are made possible by its ability to simultaneously measure the real-time effects of the atmosphere on a nearby bright guide star and correct for it on the faint target. We present the implementation of DFPR on the Keck Interferometer. Then, we detail its on-sky performance focusing on the accuracy of the turbulence correction and the resulting fringe contrast stability. © 2014. The American Astronomical Society. All rights reserved.
• {Eisner}, J., {Hillenbrand}, L., , J. (2014). "{Constraining the sub-au-scale distribution of hydrogen and carbon monoxide gas around young stars with the Keck Interferometer}". mnras, 443, 1916-1945.
• {Sheehan}, P., , J. (2014). "{Constraining the Disk Masses of the Class I Binary Protostar GV Tau}". apj, 791, 19.
• {Stone}, J., {Eisner}, J., {Salyk}, C., {Kulesa}, C., , D. (2014). "{Variable Accretion Processes in the Young Binary-star System UY Aur}". apj, 792, 56.
• {Woillez}, J., {Wizinowich}, P., {Akeson}, R., {Colavita}, M., {Eisner}, J., {Millan-Gabet}, R., {Monnier}, J., {Pott}, J., , S. (2014). "{First Faint Dual-field Off-axis Observations in Optical Long Baseline Interferometry}". apj, 783, 104.
• Plambeck, R. L., Bolatto, A. D., Carpenter, J. M., Eisner, J. A., Lamb, J. W., Leitch, E. M., Marrone, D. P., Muchovej, S. J., Pérez, L., Pound, M. W., Teuben, P. J., Volgenau, N. H., Woody, D. P., Wright, M. C., & Zauderer, B. A. (2013). THE ionized circumstellar envelopes of orion source i and the becklin-neugebauer object. Astrophysical Journal, 765(1).
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  Abstract: The 229 GHz (λ1.3 mm) radio emission from Orion-KL was mapped with up to 0.″14 angular resolution with CARMA, allowing measurements of the flux densities of Source I ("SrcI") and the Becklin-Neugebauer Object (BN), the two most massive stars in this region. We find integrated flux densities of 310 ± 45 mJy for SrcI and 240 ± 35 mJy for BN. SrcI is optically thick even at 229 GHz. No trace of the H30α recombination line is seen in its spectrum, although the v 2 = 1, 5(5,0)-6(4,3) transition of H2O, 3450 K above the ground state, is prominent. SrcI is elongated at position angle 140°, as in 43 GHz images. These results are most easily reconciled with models in which the radio emission from SrcI arises via the H- free-free opacity in a T < 4500 K disk, as considered by Reid et al. By contrast, the radio spectrum of BN is consistent with p +/e - free-free emission from a dense (ne ∼ 5 × 107 cm-3), but otherwise conventional, hypercompact H II region. The source is becoming optically thin at 229 GHz, and the H30α recombination line, at V LSR = 23.2 ± 0.5 km s-1, is prominent in its spectrum. A Lyman continuum flux of 5 × 1045 photons s-1, consistent with that expected from a B star, is required to maintain the ionization. Supplementary 90 GHz observations were made to measure the H41α and H42α recombination lines toward BN. Published 43 and 86 GHz data suggest that SrcI brightened with respect to BN over the 15 year period from 1994 to 2009. © 2013. The American Astronomical Society. All rights reserved.
• {Eisner}, J., {Rieke}, G., {Rieke}, M., {Flaherty}, K., {Arnold}, T., {Stone}, J., {Cortes}, S., {Cox}, E., {Hawkins}, C., {Cole}, A., {Zajac}, S., , A. (2013). "{Time-monitoring observations of the ro-vibrational overtone CO bands in young stars}". mnras, 434, 407-414.
• {Guyon}, O., {Eisner}, J., {Angel}, R., {Woolf}, N., {Bendek}, E., {Milster}, T., {Ammons}, S., {Shao}, M., {Shaklan}, S., {Levine}, M., {Nemati}, B., {Martinache}, F., {Pitman}, J., {Woodruff}, R., , R. (2013). "{Simultaneous Exoplanet Characterization and Deep Wide-field Imaging with a Diffractive Pupil Telescope}". apj, 767, 11.
• {Plambeck}, R., {Bolatto}, A., {Carpenter}, J., {Eisner}, J., {Lamb}, J., {Leitch}, E., {Marrone}, D., {Muchovej}, S., {P{'e}rez}, L., {Pound}, M., {Teuben}, P., {Volgenau}, N., {Woody}, D., {Wright}, M., , B. (2013). "{The Ionized Circumstellar Envelopes of Orion Source I and the Becklin-Neugebauer Object}". apj, 765, 40.
• Arnold, T. J., Eisner, J. A., Monnier, J. D., & Tuthill, P. (2012). New spatially resolved mid-infrared observations of the transitional disk TW Hya and tentative evidence for a self-luminous companion. Astrophysical Journal, 750(2).
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  Abstract: We present spatially resolved observations of the canonical transition disk object TW Hya at 8.74 μm, 11.66 μm, and 18.30 μm, obtained with the T-ReCS instrument on the Gemini telescope. These observations are a result of a novel observing mode at Gemini that enables speckle imaging. Using this technique, we image our target with short enough exposure times to achieve diffraction limited images. We use Fourier techniques to reduce our data, which allows high-precision calibration of the instrumental point-spread function. Our observations span two epochs and we present evidence for temporal variability at 11.66 μm in the disk of TW Hya. We show that previous models of TW Hya's disk from the literature are incompatible with our observations and construct a model to explain the discrepancies. We detect marginal asymmetry in our data, most significantly at the shortest wavelengths. To explain our data, we require a model that includes an optically thin inner disk extending from 0.02 to 3.9 AU, an optically thick ring representing the outer disk wall at 3.9 AU and extending to 4.6 AU, and a hotter-than-disk-equilibrium source of emission located at ∼3.5 AU. © 2012. The American Astronomical Society. All rights reserved.
• Eisner, J. A. (2012). Disk masses at the end of the main accretion phase: Carma observations and multi-wavelength modeling of class i protostars. Astrophysical Journal, 755(1).
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  Abstract: We present imaging observations at the 1.3mm wavelength of ClassI protostars in the Taurus star-forming region, obtained with the CARMA interferometer. Of an initial sample of 10 objects, we detected and imaged millimeter wavelength emission from 9. One of the nine is resolved into two sources and detailed analysis of this binary protostellar system is deferred to a future paper. For the remaining eight objects, we use the CARMA data to determine the basic morphology of the millimeter emission. Combining the millimeter data with 0.9 μm images of scattered light, Spitzer Infrared Spectrograph spectra, and broadband spectral energy distributions (all from the literature), we attempt to determine the structure of the circumstellar material. We consider models including both circumstellar disks and envelopes, and constrain the masses (and other structural parameters) of each of these components. We show that the disk masses in our sample span a range from ≲ 0.01 to ≳ 0.1 M. The disk masses for our sample are significantly higher than for samples of more evolved ClassII objects. Thus, ClassI disk masses probably provide a more accurate estimate of the initial mass budget for star and planet formation. However, the disk masses determined here are lower than required by theories of giant planet formation. The masses also appear too low for gravitational instability, which could lead to high mass accretion rates. Even in these ClassI disks, substantial particle growth may have hidden much of the disk mass in hard-to-see larger bodies. © 2012 The American Astronomical Society. All rights reserved.
• Sivanandam, S., C., R., Moon, D., Ke, M., Millar-Blanchaer, M., Eikenberry, S. S., Chun, M., Kim, S. C., Raines, S. N., & Eisner, J. (2012). The development of WIFIS: A wide integral field infrared spectrograph. Proceedings of SPIE - The International Society for Optical Engineering, 8446.
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  Abstract: We present the current results from the development of a wide integral field infrared spectrograph (WIFIS). WIFIS offers an unprecedented combination of etendue and spectral resolving power for seeing-limited, integral field observations in the 0:9 - 1:8 μm range and is most sensitive in the 0:9 - 1:35 μm range. Its optical design consists of front-end re-imaging optics, an all-reflective image slicer-type, integral field unit (IFU) called FISICA, and a long-slit grating spectrograph back-end that is coupled with a HAWAII 2RG focal plane array. The full wavelength range is achieved by selecting between two different gratings. By virtue of its re-imaging optics, the spectrograph is quite versatile and can be used at multiple telescopes. The size of its field-of-view is unrivalled by other similar spectrographs, offering a 4.5'' x 12'' integral field at a 10-meter class telescope (or 20'' x 50'' at a 2.3-meter telescope). The use of WIFIS will be crucial in astronomical problems which require wide-field, two-dimensional spectroscopy such as the study of merging galaxies at moderate redshift and nearby star/planet-forming regions and supernova remnants. We discuss the final optical design of WIFIS, and its predicted on-sky performance on two reference telescope platforms: the 2.3-m Steward Bok telescope and the 10.4-m Gran Telescopio Canarias. We also present the results from our laboratory characterization of FISICA. IFU properties such as magnification, field-mapping, and slit width along the entire slit length were measured by our tests. The construction and testing of WIFIS is expected to be completed by early 2013. We plan to commission the instrument at the 2.3-m Steward Bok telescope at Kitt Peak, USA in Spring 2013. © 2012 SPIE.
• Skemer, A. J., Hinz, P. M., Esposito, S., Burrows, A., Leisenring, J., Skrutskie, M., Desidera, S., Mesa, D., Arcidiacono, C., Mannucci, F., Rodigas, T. J., Close, L., McCarthy, D., Kulesa, C., Agapito, G., Apai, D., Argomedo, J., Bailey, V., Boutsia, K., , Briguglio, R., et al. (2012). First Light LBT AO Images of HR 8799 bcde at 1.6 and 3.3 $ mu$m: New Discrepancies between Young Planets and Old Brown Dwarfs. apj, 753, 14.
• Stone, J. M., Eisner, J. A., Monnier, J. D., Woillez, J., Wizinowich, P., Pott, J. -., & Ghez, A. M. (2012). Disentangling confused stars at the galactic center with long-baseline infrared interferometry. Astrophysical Journal, 754(2).
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  Abstract: We present simulations of Keck Interferometer ASTRA and VLTI GRAVITY observations of mock star fields in orbit within 50mas of SgrA*. Dual-field phase referencing techniques, as implemented on ASTRA and planned for GRAVITY, will provide the sensitivity to observe SgrA* with long-baseline infrared interferometers. Our results show an improvement in the confusion noise limit over current astrometric surveys, opening a window to study stellar sources in the region. Since the Keck Interferometer has only a single baseline, the improvement in the confusion limit depends on source position angles. The GRAVITY instrument will yield a more compact and symmetric point-spread function, providing an improvement in confusion noise which will not depend as strongly on position angle. Our Keck results show the ability to characterize the star field as containing zero, few, or many bright stellar sources. We are also able to detect and track a source down to m K 18 through the least confused regions of our field of view at a precision of 200 μas along the baseline direction. This level of precision improves with source brightness. Our GRAVITY results show the potential to detect and track multiple sources in the field. GRAVITY will perform 10 μas astrometry on an m K = 16.3 source and 200 μas astrometry on an m K = 18.8 source in 6 hr of monitoring a crowded field. Monitoring the orbits of several stars will provide the ability to distinguish between multiple post-Newtonian orbital effects, including those due to an extended mass distribution around SgrA* and to low-order general relativistic effects. ASTRA and GRAVITY both have the potential to detect and monitor sources very close to SgrA*. Early characterizations of the field by ASTRA, including the possibility of a precise source detection, could provide valuable information for future GRAVITY implementation and observation. © 2012. The American Astronomical Society. All rights reserved..
• Woillez, J., Akeson, R., Colavita, M., Eisner, J., Millan-Gabet, R., Monnier, J., Pott, J. -., Ragland, S., Wizinowich, P., Abajian, M., Appleby, E., Berkey, B., Cooper, A., Felizardo, C., Herstein, J., Hrynevych, M., Medeiros, D., Morrison, D., Panteleeva, T., , Smith, B., et al. (2012). Self-phase-referenced spectro-interferometry on the Keck interferometer. Publications of the Astronomical Society of the Pacific, 124(911), 51-61.
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  Abstract: As part of the astrometric and phase-referenced astronomy (ASTRA) project, three new science modes are being developed for the Keck Interferometer that extend the science capabilities of this instrument to include higher spectral resolution, fainter magnitudes, and astrometry. We report on the successful implementation of the first of these science modes, the self-phase-referencing mode, which provides a K-band (λ = 2:2 μm) spectral resolution of R ∼ 1000 on targets as faint as 7.8 mag with spatial resolution as fine as λ/B = 5 mas in the K band, with the 85 m interferometer baseline. This level of spectral resolution would not have been possible without a phase-referencing implementation extending the integration time limit imposed by atmospheric turbulence. For narrow spectral features, we demonstrate a precision of ±0:01 on the differential V 2(λ), and ±1:7 mrad on the differential phase Φ(λ), equivalent to a differential astrometry precision of ±1:45 μas. This new Keck Interferometer instrument is typically used to study the geometry and location of narrow spectral features at high angular resolution, referenced to a continuum. By simultaneously providing spectral and spatial information, the geometry of velocity fields (e.g., rotating disks, inflows, outflows, etc.) larger than 150 km s -1 can also be explored. © 2012. The Astronomical Society of the Pacific. All rights reserved.
• Woillez, J., Wizinowich, P., Akeson, R., Colavita, M., Eisner, J., Millan-Gabet, R., Monnier, J., Pott, J. -., Ragland, S., Appleby, E., Cooper, A., Felizardo, C., Herstein, J., Martin, O., Medeiros, D., Morrison, D., Panteleeva, T., Smith, B., Summers, K., , Tsubota, K., et al. (2012). First faint Dual-Field Phase-Referenced observations on the Keck Interferometer. Proceedings of SPIE - The International Society for Optical Engineering, 8445.
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  Abstract: Ground-based long baseline interferometers have long been limited in sensitivity by the short integration periods imposed by atmospheric turbulence. The first observation fainter than this limit was performed on January 22, 2011 when the Keck Interferometer observed a K=11.5 target, about one magnitude fainter than its K=10.3 limit. This observation was made possible by the Dual Field Phase Referencing instrument of the ASTRA project: simultaneously measuring the real-time effects of the atmosphere on a nearby bright guide star, and correcting for it on the faint target, integration time longer than the turbulence time scale are made possible. As a prelude tóthis demonstration, we first present the implementation of Dual Field Phase Referencing on the interferometer. We then detail its on-sky performance focusing on the accuracy of the turbulence correction, and on the resulting fringe contrast stability. We conclude with a presentation of early results obtained with Laser Guide Star AO and the interferometer. © 2012 SPIE.
• {Arnold}, T., {Eisner}, J., {Monnier}, J., , P. (2012). "{New Spatially Resolved Mid-infrared Observations of the Transitional Disk TW Hya and Tentative Evidence for a Self-luminous Companion}". apj, 750, 119.
• {Eisner}, J. (2012). "{Disk Masses at the End of the Main Accretion Phase: CARMA Observations and Multi-wavelength Modeling of Class I Protostars}". apj, 755, 23.
• {Guyon}, O., {Bendek}, E., {Eisner}, J., {Angel}, R., {Woolf}, N., {Milster}, T., {Ammons}, S., {Shao}, M., {Shaklan}, S., {Levine}, M., {Nemati}, B., {Pitman}, J., {Woodruff}, R., , R. (2012). "{High-precision Astrometry with a Diffractive Pupil Telescope}". apjs, 200, 11.
• {Rodigas}, T., {Hinz}, P., {Leisenring}, J., {Vaitheeswaran}, V., {Skemer}, A., {Skrutskie}, M., {Su}, K., {Bailey}, V., {Schneider}, G., {Close}, L., {Mannucci}, F., {Esposito}, S., {Arcidiacono}, C., {Pinna}, E., {Argomedo}, J., {Agapito}, G., {Apai}, D., {Bono}, G., {Boutsia}, K., , {Briguglio}, R., et al. (2012). "{The Gray Needle: Large Grains in the HD 15115 Debris Disk from LBT/PISCES/Ks and LBTI/LMIRcam/L' Adaptive Optics Imaging}". apj, 752, 57.
• {Skemer}, A., {Hinz}, P., {Esposito}, S., {Burrows}, A., {Leisenring}, J., {Skrutskie}, M., {Desidera}, S., {Mesa}, D., {Arcidiacono}, C., {Mannucci}, F., {Rodigas}, T., {Close}, L., {McCarthy}, D., {Kulesa}, C., {Agapito}, G., {Apai}, D., {Argomedo}, J., {Bailey}, V., {Boutsia}, K., , {Briguglio}, R., et al. (2012). "{First Light LBT AO Images of HR 8799 bcde at 1.6 and 3.3 {$mu$}m: New Discrepancies between Young Planets and Old Brown Dwarfs}". apj, 753, 14.
• {Stone}, J., {Eisner}, J., {Monnier}, J., {Woillez}, J., {Wizinowich}, P., {Pott}, J., , A. (2012). "{Disentangling Confused Stars at the Galactic Center with Long-baseline Infrared Interferometry}". apj, 754, 151.
• {Woillez}, J., {Akeson}, R., {Colavita}, M., {Eisner}, J., {Millan-Gabet}, R., {Monnier}, J., {Pott}, J., {Ragland}, S., {Wizinowich}, P., {Abajian}, M., {Appleby}, E., {Berkey}, B., {Cooper}, A., {Felizardo}, C., {Herstein}, J., {Hrynevych}, M., {Medeiros}, D., {Morrison}, D., {Panteleeva}, T., , {Smith}, B., et al. (2012). "{Self-Phase-Referenced Spectro-Interferometry on the Keck Interferometer}". pasp, 124, 51-61.
• Eisner, J. A., & Hillenbrand, L. A. (2011). Resolving the SUB-AU-SCALE gas and dust distribution in FU Orionis sources. Astrophysical Journal, 738(1).
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  Abstract: We present Keck Interferometer observations of the three prototypical FU Orionis stars, FU Ori, V1057Cyg, and V1515Cyg. With a spatial resolution of a few milliarcseconds and a spectral resolution of λ/Δλ = 2000, our near-infrared observations spatially resolve gas and dust emission extending from stellocentric radii of 0.05AU to several AU. We fit these data with accretion disk models where each stellocentric radius of the disk is represented by a supergiant-type stellar emission spectrum at the disk temperature. A disk model is consistent with the data for FU Ori, although we require some local asymmetry in the disk. For V1057Cyg the disk model does not fit our data well, especially compared to the fit quality achieved for FU Ori. We speculate that a disk wind may be contributing substantially to the observed near-IR emission in this source. The data for V1515Cyg are noisier than the data obtained for the other two objects and do not strongly constrain the validity of an accretion disk model. © 2011. The American Astronomical Society. All rights reserved.
• {Eisner}, J., , L. (2011). "{Resolving the Sub-AU-scale Gas and Dust Distribution in FU Orionis Sources}". apj, 738, 9.
• Eisner, J. A., Akeson, R., Colavita, M., Ghez, A., Graham, J., Hillenbrand, L., Millan-Gabet, R., Monnier, J. D., Pott, J. -., Ragland, S., Wizinowich, P., & Woillez, J. (2010). Science with the Keck Interferometer ASTRA program. Proceedings of SPIE - The International Society for Optical Engineering, 7734.
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  Abstract: The ASTrometric and phase-Referenced Astronomy (ASTRA) project will provide phase referencing and astrometric observations at the Keck Interferometer, leading to enhanced sensitivity and the ability to monitor orbits at an accuracy level of 30-100 microarcseconds. Here we discuss recent scientific results from ASTRA, and describe new scientific programs that will begin in 2010-2011. We begin with results from the "self phase referencing" (SPR) mode of ASTRA, which uses continuum light to correct atmospheric phase variations and produce a phase-stabilized channel for spectroscopy. We have observed a number of protoplanetary disks using SPR and a grism providing a spectral dispersion of ∼ 2000. In our data we spatially resolve emission from dust as well as gas. Hydrogen line emission is spectrally resolved, allowing differential phase measurements across the emission line that constrain the relative centroids of different velocity components at the 10 microarcsecond level. In the upcoming year, we will begin dual-field phase referencing (DFPR) measurements of the Galactic Center and a number of exoplanet systems. These observations will, in part, serve as precursors to astrometric monitoring of stellar orbits in the Galactic Center and stellar wobbles of exoplanet host stars. We describe the design of several scientific investigations capitalizing on the upcoming phase-referencing and astrometric capabilities of ASTRA. © 2010 SPIE.
• Eisner, J. A., Monnier, J. D., Woillez, J., Akeson, R. L., Millan-Gabet, R., Graham, J. R., Hillenbr, L. A., Pott, J. -., Ragland, S., & Wizinowich, P. (2010). Spatially and spectrally resolved hydrogen gas within 0.1 Au of T Tauri and herbig Ae/Be stars. Astrophysical Journal Letters, 718(2), 774-794.
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  Abstract: We present near-infrared observations of T Tauri and Herbig Ae/Be stars with a spatial resolution of a few milliarcseconds and a spectral resolution of ∼2000. Our observations spatially resolve gas and dust in the inner regions of protoplanetary disks, and spectrally resolve broad-linewidth emission from the Brγ transition of hydrogen gas. We use the technique of spectro-astrometry to determine centroids of different velocity components of this gaseous emission at a precision orders of magnitude better than the angular resolution. In all sources, we find the gaseous emission to be more compact than or distributed on similar spatial scales to the dust emission. We attempt to fit the data with models including both dust and Brγ -emitting gas, and we consider both disk and infall/outflow morphologies for the gaseous matter. In most cases where we can distinguish between these two models, the data show a preference for infall/outflow models. In all cases, our data appear consistent with the presence of some gas at stellocentric radii of ∼0.01 AU. Our findings support the hypothesis that Brγ emission generally traces magnetospherically driven accretion and/or outflows in young star/disk systems. © 2010. The American Astronomical Society. All rights reserved.
• Pott, J. -., Woillez, J., Ragland, S., Wizinowich, P. L., Eisner, J. A., Monnier, J. D., Akeson, R. L., Ghez, A. M., Graham, J. R., Hillenbrand, L. A., Millan-Gabet, R., Appleby, E., Berkey, B., Colavita, M. M., Cooper, A., Felizardo, C., Herstein, J., Hrynevych, M., Medeiros, D., , Morrison, D., et al. (2010). First Keck interferometer measurements in self-phase referencing mode: Spatially resolving circum-stellar line emission of 48 Lib. Proceedings of SPIE - The International Society for Optical Engineering, 7734.
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  Abstract: Recently, the Keck interferometer was upgraded to do self-phase-referencing (SPR) assisted K-band spectroscopy at R ∼ 2000. This means, combining a spectral resolution of 150 km/s with an angular resolution of 2.7 mas, while maintaining high sensitiviy. This SPR mode operates two fringe trackers in parallel, and explores several infrastructural requirements for off-axis phase-referencing, as currently being implemented as the KI-ASTRA project. The technology of self-phasereferencing opens the way to reach very high spectral resolution in near-infrared interferometry. We present the scientific capabilities of the KI-SPR mode in detail, at the example of observations of the Be-star 48 Lib. Several spectral lines of the cirumstellar disk are resolved. We describe the first detection of Pfund-lines in an interferometric spectrum of a Be star, in addition to Br γ . The differential phase signal can be used to (i) distinguish circum-stellar line emission from the star, (ii) to directly measure line asymmetries tracing an asymetric gas density distribution, (iii) to reach a differential, astrometric precision beyond single-telescope limits sufficient for studying the radial disk structure. Our data support the existence of a radius-dependent disk density perturbation, typically used to explain slow variations of Be-disk hydrogen line profiles. © 2010 SPIE.
• Pott, J. -., Woillez, J., Ragland, S., Wizinowich, P. L., Eisner, J. A., Monnier, J. D., Akeson, R. L., Ghez, A. M., Graham, J. R., Hillenbrand, L. A., Millan-Gabet, R., Appleby, E., Berkey, B., Colavita, M. M., Cooper, A., Felizardo, C., Herstein, J., Hrynevych, M., Medeiros, D., , Morrison, D., et al. (2010). Probing local density inhomogeneities in the circumstellar disk of a be star using the new spectro-astrometry mode at the Keck Interferometer. Astrophysical Journal Letters, 721(1), 802-808.
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  Abstract: We report on the successful science verification phase of a new observing mode at the Keck Interferometer, which provides a line-spread function width and sampling of 150 km s-1 at the K-band, at a current limiting magnitude of K- ∼ 7 mag with a spatial resolution of λ/2B ≈ 2.7mas and a measured differential phase stability of unprecedented precision (3 mrad at K = 5mag, which represents 3μ as on the sky or a centroiding precision of 10-3). The scientific potential of this mode is demonstrated by the presented observations of the circumstellar disk of the evolved Be-star 48 Lib. In addition to indirect methods such as multi-wavelength spectroscopy and polarimetry, the spectro-interferometric astrometry described here provides a new tool to directly constrain the radial density structure in the disk. For the first time, we resolve several Pfund emission lines, in addition to Br γ, in a single interferometric spectrum, with adequate spatial and spectral resolution and precision to analyze the radial disk structure in 48 Lib. The data suggest that the continuum and Pf -emission originates in significantly more compact regions, inside the Br γ -emission zone. Thus, spectro-interferometric astrometry opens the opportunity to directly connect the different observed line profiles of Br γ and Pfund in the total and correlated flux to different disk radii. The gravitational potential of a rotationally flattened Be star is expected to induce a one-armed density perturbation in the circumstellar disk. Such a slowly rotating disk oscillation has been used to explain the well-known periodic V/R spectral profile variability in these stars, as well as the observed V/R cycle phase shifts between different disk emission lines. The differential line properties and linear constraints set by our data are consistent with theoretical models and lend direct support to the existence of a radius-dependent disk density perturbation. The data also show decreasing gas rotation velocities at increasing stellocentric radii as expected for Keplerian disk rotation, assumed by those models. © 2010. The American Astronomical Society. All rights reserved.
• Woillez, J., Akeson, R., Colavita, M., Eisner, J., Ghez, A., Graham, J., Hillenbrand, L., Millan-Gabet, R., Monnier, J., Pott, J. -., Ragland, S., Wizinowich, P., Appleby, E., Berkey, B., Cooper, A., Felizardo, C., Herstein, J., Hrynevych, M., Martin, O., , Medeiros, D., et al. (2010). ASTRA: ASTrometry and phase-Referencing Astronomy on the Keck interferometer. Proceedings of SPIE - The International Society for Optical Engineering, 7734.
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  Abstract: ASTRA (ASTrometric and phase-Referencing Astronomy) is an upgrade to the existing Keck Interferometer which aims at providing new self-phase referencing (high spectral resolution observation of YSOs), dual-field phase referencing (sensitive AGN observations), and astrometric (known exoplanetary systems characterization and galactic center general relativity in strong field regime) capabilities. With the first high spectral resolution mode now offered to the community, this contribution focuses on the progress of the dual field and astrometric modes. © 2010 SPIE.
• {Eisner}, J., {Doppmann}, G., {Najita}, J., {McCarthy}, D., {Kulesa}, C., {Swift}, B., , J. (2010). "{Time-variable Accretion in the TW Hya Star/disk System}". apjl, 722, L28-L32.
• {Eisner}, J., {Monnier}, J., {Woillez}, J., {Akeson}, R., {Millan-Gabet}, R., {Graham}, J., {Hillenbrand}, L., {Pott}, J., {Ragland}, S., , P. (2010). "{Spatially and Spectrally Resolved Hydrogen Gas within 0.1 AU of T Tauri and Herbig Ae/Be Stars}". apj, 718, 774-794.
• {Pott}, J., {Woillez}, J., {Ragland}, S., {Wizinowich}, P., {Eisner}, J., {Monnier}, J., {Akeson}, R., {Ghez}, A., {Graham}, J., {Hillenbrand}, L., {Millan-Gabet}, R., {Appleby}, E., {Berkey}, B., {Colavita}, M., {Cooper}, A., {Felizardo}, C., {Herstein}, J., {Hrynevych}, M., {Medeiros}, D., , {Morrison}, D., et al. (2010). "{Probing Local Density Inhomogeneities in the Circumstellar Disk of a Be Star Using the New Spectro-astrometry Mode at the Keck Interferometer}". apj, 721, 802-808.
• Eisner, J. A., Graham, J. R., Akeson, R. L., & Najita, J. (2009). Spatially resolved spectroscopy of sub-au-sized regions of T tauri and Herbig AE/BE disks. Astrophysical Journal, 692(1), 309-323.
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  Abstract: We present spatially resolved near-IR spectroscopic observations of 15 young stars. Using a grism spectrometer behind the Keck interferometer, we obtained an angular resolution of a few milliarcseconds and a spectral resolution of 230, enabling probes of both gas and dust in the inner disks surrounding the target stars. We find that the angular size of the near-IR emission typically increases with wavelength, indicating hot, presumably gaseous material within the dust sublimation radius. Our data also clearly indicate Brγ emission arising from hot hydrogen gas, and suggest the presence of water vapor and carbon monoxide gas in the inner disks of several objects. This gaseous emission is more compact than the dust continuum emission in all cases. We construct simple physical models of the inner disk and fit them to our data to constrain the spatial distribution and temperature of dust and gas emission components. © 2009. The American Astronomical Society. All rights reserved.
• Eisner, J. A., Monnier, J. D., Tuthill, P., & Lacour, S. (2009). Spatially resolved mid-infrared imaging of the SR 21 transition disk. Astrophysical Journal, 698(2), L169-L173.
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  Abstract: We present mid-infrared (mid-IR) observations from Gemini /TReCS that spatially resolve the dust emission around SR 21. The protoplanetary disk around SR 21 is believed to have a cleared gap extending from stellocentric radii of ∼0.5 AU to ∼20 AU, based on modeling of the observed spectral energy distribution (SED). Our new observations resolve the dust emission, and our data are inconsistent with the previous model. We require the disk to be completely cleared within ∼10 AU, without the hot inner disk spanning ∼0.25-0.5 AU posited previously. To fit the SED and mid-IR imaging data together, we propose a disk model with a large inner hole, but with a warm companion - possibly surrounded by circumstellar material of its own - residing near the outer edge of the cleared region. We also discuss a model with a narrow ring included in a large cleared inner disk region, and argue that it is difficult to reconcile with the data. © 2009. The American Astronomical Society. All rights reserved.
• Hełminiak, K., Konacki, M., Kulkarni, S. R., & Eisner, J. (2009). Precision astrometry of a sample of speckle binaries and multiples with the adaptive optics facilities at the Hale and Keck II telescopes. Monthly Notices of the Royal Astronomical Society, 400(1), 406-421.
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  Abstract: Using the adaptive optics facilities at the 200-in Hale and 10-m Keck II, we observed in the near-infrared a sample of 12 binary and multiple stars and one open cluster. We used the near diffraction limited images of these systems to measure the relative separations and position angles between their components. In this paper, we investigate and correct for the influence of the differential chromatic refraction and chip distortions on our relative astrometric measurements. Over one night, we achieve an astrometric precision typically well below 1 mas and occasionally as small as 40 μas. Such a precision is in principle sufficient to astrometrically detect planetary mass objects around the components of nearby binary and multiple stars. Since we have not had sufficiently large data sets for the observed sample of stars to detect planets, we provide the limits to planetary mass objects based on the obtained astrometric precision. © 2009 RAS.
• Najita, J. R., Doppmann, G. W., Carr, J. S., Graham, J. R., & Eisner, J. A. (2009). High-resolution k-band spectroscopy of MWC 480 and V1331 Cyg. Astrophysical Journal, 691(1), 738-748.
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  Abstract: We present high-resolution (R = 25,000-35,000) K-band spectroscopy of two young stars, MWC 480 and V1331 Cyg. Earlier spectrally dispersed (R = 230) interferometric observations of MWC 480 indicated the presence of an excess continuum emission interior to the dust sublimation radius, with a spectral shape that was interpreted as evidence for hot water emission from the inner disk of MWC 480. Our spectrum of V1331 Cyg reveals strong emission from CO and hot water vapor, likely arising in a circumstellar disk. In comparison, our spectrum of MWC 480 appears mostly featureless. We discuss possible ways in which strong water emission from MWC 480 might go undetected in our data. If strong water emission is in fact absent from the inner disk, as our data suggest, the continuum excess interior to the dust sublimation radius that is detected in the interferometric data must have another origin. We discuss possible physical origins for the continuum excess. © 2009. The American Astronomical Society. All rights reserved.
• Pott, J., Woillez, J., Akeson, R. L., Berkey, B., Colavita, M. M., Cooper, A., Eisner, J. A., Ghez, A. M., Graham, J. R., Hillenbrand, L., Hrynewych, M., Medeiros, D., Millan-Gabet, R., Monnier, J., Morrison, D., Panteleeva, T., Quataert, E., Randolph, B., Smith, B., , Summers, K., et al. (2009). Astrometry with the Keck Interferometer: The ASTRA project and its science. New Astronomy Reviews, 53(11-12), 363-372.
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  Abstract: The sensitivity and astrometry upgrade ASTRA of the Keck Interferometer is introduced. After a brief overview of the underlying interferometric principles, the technology and concepts of the upgrade are presented. The interferometric dual-field technology of ASTRA will provide the KI with the means to observe two objects simultaneously, and measure the distance between them with a precision eventually better than 100 μas. This astrometric functionality of ASTRA will add a unique observing tool to fields of astrophysical research as diverse as exo-planetary kinematics, binary astrometry, and the investigation of stars accelerated by the massive black hole in the center of the Milky Way as discussed in this contribution. © 2010 Elsevier B.V.
• {Eisner}, J., {Graham}, J., {Akeson}, R., , J. (2009). "{Spatially Resolved Spectroscopy of Sub-AU-Sized Regions of T Tauri and Herbig Ae/Be Disks}". apj, 692, 309-323.
• {Eisner}, J., {Monnier}, J., {Tuthill}, P., , S. (2009). "{Spatially Resolved Mid-Infrared Imaging of the SR 21 Transition Disk}". apjl, 698, L169-L173.
• {He{l}miniak}, K., {Konacki}, M., {Kulkarni}, S., , J. (2009). "{Precision astrometry of a sample of speckle binaries and multiples with the adaptive optics facilities at the Hale and Keck II telescopes}". mnras, 400, 406-421.
• {Najita}, J., {Doppmann}, G., {Carr}, J., {Graham}, J., , J. (2009). "{High-Resolution K-Band Spectroscopy of MWC 480 and V1331 Cyg}". apj, 691, 738-748.
• {Pott}, J., {Woillez}, J., {Akeson}, R., {Berkey}, B., {Colavita}, M., {Cooper}, A., {Eisner}, J., {Ghez}, A., {Graham}, J., {Hillenbrand}, L., {Hrynewych}, M., {Medeiros}, D., {Millan-Gabet}, R., {Monnier}, J., {Morrison}, D., {Panteleeva}, T., {Quataert}, E., {Randolph}, B., {Smith}, B., , {Summers}, K., et al. (2009). "{Astrometry with the Keck Interferometer: The ASTRA project and its science}". nar, 53, 363-372.
• Eisner, J. A., Plambeck, R. L., Carpenter, J. M., Corder, S. A., Qi, C., & Wilner, D. (2008). Proplyds and massive disks in the Orion nebula cluster imaged with CARMA and SMA. Astrophysical Journal, 683(1), 304-320.
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  Abstract: We imaged a 2′ x 2′ region of the Orion Nebula Cluster (ONC) in 1.3 mm wavelength continuum emission with the recently commissioned Combined Array for Research in Millimeter Astronomy (CARMA) and with the Submillimeter Array (SMA). Our mosaics include >250 known near-IR cluster members, of which 36 are so-called "proplyds" that have been imaged previously with the Hubble Space Telescope. We detected 40 sources in 1 mm continuum emission (one of which is the BN Object), and several of them are spatially resolved with our observations. The emission from most objects arises predominantly from dust, and circumstellar masses inferred for detected sources range from 0.01 to 0.5 Modot;. The average circumstellar mass for undetected sources is estimated to be ∼0.001 M⊙, approximately an order of magnitude smaller than the minimum-mass solar nebula. Most stars in the ONC thus do not appear to currently possess sufficient mass in small dust grains to form Jupiter-mass (or larger) planets. Comparison with previous results for younger and older regions indicates that massive disks evolve significantly on ∼Myr timescales. We also show that the percentage of stars in Orion surrounded by disks more massive than ∼0.01 M⊙ is substantially lower than in Taurus, indicating that environment has an impact on the disk-mass distribution. Disks in Orion may be truncated through photoevaporation caused by the intense radiation field of the Trapezium stars, and we see marginal evidence for such a scenario in the spatial distribution of massive disks within the cluster. Our data show no statistically significant correlation between disk and stellar masses, although we see hints of a higher percentage of massive disks around lower mass stars. © 2008. The American Astronomical Society. All rights reserved.
• {Eisner}, J., {Plambeck}, R., {Carpenter}, J., {Corder}, S., {Qi}, C., , D. (2008). "{Proplyds and Massive Disks in the Orion Nebula Cluster Imaged with CARMA and SMA}". apj, 683, 304-320.
• Eisner, J. A. (2007). Water vapour and hydrogen in the terrestrial-planet-forming region of a protoplanetary disk. Nature, 447(7144), 562-564.
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  PMID: 17538613;Abstract: Planetary systems (ours included) formed in disks of dust and gas around young stars. Disks are an integral part of the star and planet formation process, and knowledge of the distribution and temperature of inner-disk material is crucial for understanding terrestrial planet formation, giant planet migration, and accretion onto the central star. Although the inner regions of protoplanetary disks in nearby star-forming regions subtend only a few nano-radians, near-infrared interferometry has recently enabled the spatial resolution of these terrestrial zones. Most observations have probed only dust, which typically dominates the near-infrared emission. Here I report spectrally dispersed near-infrared interferometric observations that probe the gas (which dominates the mass and dynamics of the inner disk), in addition to the dust, within one astronomical unit (1 au, the Sun-Earth distance) of the young star MWC 480. I resolve gas, including water vapour and atomic hydrogen, interior to the edge of the dust disk; this contrasts with results of previous spectrally dispersed interferometry observations. Interactions of this accreting gas with migrating planets may lead to short-period exoplanets like those detected around main-sequence stars. The observed water vapour is probably produced by the sublimation of migrating icy bodies, and provides a potential reservoir of water for terrestrial planets. ©2007 Nature Publishing Group.
• Eisner, J. A., Chiang, E. I., Lane, B. P., & Akeson, R. L. (2007). Spectrally dispersed K-band interferometric observations of herbig Ae/Be sources: Inner disk temperature profiles. Astrophysical Journal, 657(1 I), 347-358.
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  Abstract: We use spectrally dispersed near-IR interferometry data to constrain the temperature profiles of sub-AU-sized regions of 11 Herbig Ae/Be sources. We find that a single-temperature ring does not reproduce the data well. Rather, models incorporating radial temperature gradients are preferred. These gradients may arise in a dusty disk, or may reflect separate gas and dust components with different temperatures and spatial distributions. Comparison of our models with broad-band spectral energy distributions suggests the latter explanation. The data support the view that the near-IR emission of Herbig Ae/Be sources arises from hot circumstellar dust and gas in sub-AU-sized disk regions. Intriguingly, our derived temperature gradients appear systematically steeper for disks around higher mass stars. It is not clear, however, whether this reflects trends in relative dust/gas contributions or gradients within individual components. © 2007, The American Astronomical Society. All rights reserved.
• Eisner, J. A., Graham, J. R., Akeson, R. L., Ligon, E. R., Colavita, M. M., Basri, G., Summers, K., Ragland, S., & Booth, A. (2007). Stellar and molecular radii of a Mira star: First observations with the Keck Interferometer grism. Astrophysical Journal, 654(1 II), L77-L80.
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  Abstract: Using a new grism at the Keck Interferometer, we obtained spectrally dispersed (R ∼ 230) interferometric measurements of the Mira star R Vir. These data show that the measured radius of the emission varies substantially from 2.0 to 2.4 μm. Simple models can reproduce these wavelength-dependent variations using extended molecular layers, which absorb stellar radiation and reemit it at longer wavelengths. Because we observe spectral regions with and without substantial molecular opacity, we determine the stellar photospheric radius, uncontaminated by molecular emission. We infer that most of the molecular opacity arises at approximately twice the radius of the stellar photosphere. © 2007. The American Astronomical Society. All rights reserved.
• Eisner, J. A., Hillenbrand, L. A., White, R. J., Bloom, J. S., Akeson, R. L., & Blake, C. H. (2007). Near-infrared interferometric, spectroscopic, and photometric monitoring of T Tauri inner disks. Astrophysical Journal, 669(2), 1072-1084.
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  Abstract: We present high angular resolution observations with the Keck Interferometer, high-dispersion spectroscopic observations with Keck/NIRSPEC, and near-IR photometric observations from PAIRITEL of a sample of 11 solar-type T Tauri stars in nine systems. We use these observations to probe the circumstellar material within 1 AU of these young stars, measuring the circumstellar-to-stellar flux ratios and angular size scales of the 2.2 μm emission. Our sample spans a range of stellar luminosities and mass accretion rates, allowing investigation of potential correlations between inner disk properties and stellar or accretion properties. We suggest that the mechanism by which the dusty inner disk is truncated may depend on the accretion rate of the source; in objects with low accretion rates, the stellar magnetospheres may truncate the disks, while sublimation may truncate dusty disks around sources with higher accretion rates. We have also included in our sample objects that are known to be highly variable (based on previous photometric and spectroscopic observations), and for several sources, we obtained multiple epochs of spectroscopic and interferometrie data, supplemented by near-IR photometric monitoring, to search for inner disk variability. While time-variable veilings and accretion rates are observed in some sources, no strong evidence for inner disk pulsation is found. © 2007. The American Astronomical Society. All rights reserved.
• Lane, B. F., Retter, A., Eisner, J. A., Muterspaugh, M. W., Thompson, R. R., & Sokoloski, J. L. (2007). Interferometric observations of V1663 Aquilae (nova AQL 2005). Astrophysical Journal, 669(2), 1150-1155.
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  Abstract: We have resolved the classical nova V1663 Aql using long-baseline near-IR interferometry covering the period from ∼5 to 18 days after peak brightness. We directly measure the shape and size of the fireball, which we find to be asymmetric. In addition, we measure an apparent expansion rate of 0.21 ± 0.03 mas day-1. Assuming a linear expansion model, we infer a time of initial outburst approximately 4 days prior to peak brightness. When combined with published spectroscopic expansion velocities, our angular expansion rate implies a distance of 8.9 ± 3.6 kpc. This distance measurement is independent of, but consistent with, determinations made using widely available photometric relations for novae. © 2007. The American Astronomical Society. All rights reserved.
• Lane, B. F., Sokoloski, J. L., Barry, R. K., Traub, W. A., Retter, A., Muterspaugh, M. W., Thompson, R. R., Eisner, J. A., Serabyn, E., & Mennesson, B. (2007). Interferometric observations of RS ophiuchi and the origin of the near-infrared emission. Astrophysical Journal, 658(1 I), 520-524.
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  Abstract: We report observations of the recurrent nova RS Oph using long-baseline near-IR interferometry. We are able to resolve emission from the nova for several weeks after the 2006 February outburst. The near-IR source initially expands to a size of ∼5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching ∼2 mas by day 100. We combine our measured angular diameters with previously available interferometric and photometric data to derive an emission measure for the source, and hence are able to determine the mass-loss rate of the nova in the days following the outburst. © 2007. The American Astronomical Society. All rights reserved.
• {Eisner}, J. (2007). "{Water vapour and hydrogen in the terrestrial-planet-forming region of a protoplanetary disk}". nat, 447, 562-564.
• {Eisner}, J., {Chiang}, E., {Lane}, B., , R. (2007). "{Spectrally Dispersed K-Band Interferometric Observations of Herbig Ae/Be Sources: Inner Disk Temperature Profiles}". apj, 657, 347-358.
• {Eisner}, J., {Graham}, J., {Akeson}, R., {Ligon}, E., {Colavita}, M., {Basri}, G., {Summers}, K., {Ragland}, S., , A. (2007). "{Stellar and Molecular Radii of a Mira Star: First Observations with the Keck Interferometer Grism}". apjl, 654, L77-L80.
• {Eisner}, J., {Hillenbrand}, L., {White}, R., {Bloom}, J., {Akeson}, R., , C. (2007). "{Near-Infrared Interferometric, Spectroscopic, and Photometric Monitoring of T Tauri Inner Disks}". apj, 669, 1072-1084.
• {Lane}, B., {Retter}, A., {Eisner}, J., {Muterspaugh}, M., {Thompson}, R., , J. (2007). "{Interferometric Observations of V1663 Aquilae (Nova Aql 2005)}". apj, 669, 1150-1155.
• {Lane}, B., {Sokoloski}, J., {Barry}, R., {Traub}, W., {Retter}, A., {Muterspaugh}, M., {Thompson}, R., {Eisner}, J., {Serabyn}, E., , B. (2007). "{Interferometric Observations of RS Ophiuchi and the Origin of the Near-Infrared Emission}". apj, 658, 520-524.
• Eisner, J. A., & Carpenter, J. M. (2006). Massive protoplanetary disks in the trapezium region. Astrophysical Journal Letters, 641(2 I), 1162-1171.
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  Abstract: We determine the disk mass distribution around 336 stars in the young (∼1 Myr) Orion Nebula cluster by imaging a 2.′5 × 2.′5 region in 3 mm continuum emission with the Owens Valley Millimeter Array. For this sample of 336 stars, we observe 3 mm emission above the 3 σ noise level toward 10 sources, six of which have also been detected optically in silhouette against the bright nebular background. In addition, we detect 20 objects in 3 mm continuum emission that do not correspond to known near-IR cluster members. Comparisons of our measured fluxes with longer wavelength observations enable rough separation of dust emission from thermal free-free emission, and we find substantial dust emission toward most objects. For the sample of 10 objects detected at both 3 mm and near-IR wavelengths, eight exhibit substantial dust emission. Excluding the two high-mass stars (θ1 Ori A and the BN object) and assuming a gas-to-dust ratio of 100, we estimate circumstellar masses ranging from 0.13 to 0.39 M ⊙ For the cluster members not detected at 3 mm, images of individual objects are stacked to constrain the mean 3 mm flux of the ensemble. The average flux is detected at the 3 σ confidence level and implies an average disk mass of 0.005 M⊙, comparable to the minimum-mass solar nebula. The percentage of stars in Orion surrounded by disks more massive than ∼0.1 M⊙ is consistent with the disk mass distribution in Taurus, and we argue that massive disks in Orion do not appear to be truncated through close encounters with high-mass stars. Comparison of the average disk mass and number of massive dusty structures in Orion with similar surveys of the NGC 2024 and IC 348 clusters is used to constrain the evolutionary timescales of massive circumstellar disks in clustered environments. © 2006. The American Astronomical Society. All rights reserved.
• Eisner, J. A., Chiang, E. I., & Hlllenbrand, L. A. (2006). Spatially resolving the inner disk of TW hydrae. Astrophysical Journal Letters, 637(2 II), L133-L136.
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  Abstract: We present Keck Interferometer observations of TW Hya that spatially resolve its emission at 2 μm wavelength. Analyzing these data together with existing K-band veiling and near-infrared photometric measurements, we conclude that the inner disk consists of optically thin, submicron-sized dust extending from ∼4 AU to within 0.06 AU of the central star. The inner disk edge may be magnetospherically truncated. Even if we account for the presence of gas in the inner disk, these small dust grains have survival times against radiation blowout that are orders of magnitude shorter than the age of the system, suggesting continual replenishment through collisions of larger bodies. © 2006. The American Astronomical Society. All rights reserved.
• Lane, B. F., Retter, A., Eisner, J. A., Thompson, R. R., & Muterspaugh, M. W. (2006). Interferometric observations of explosive variables: V838 mon, nova Aql 2005 & RS Oph. Proceedings of SPIE - The International Society for Optical Engineering, 6268 I.
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  Abstract: During the last two years we have used the Palomar Testbed Interferometer to observe several explosive variable stars, including V838 Monocerotis, V1663 Aquilae and recently RS Ophiuchi. We observed V838 Monocerotis approximately 34 months after its eruption, and were able to resolve the ejecta. Observations of V1663 Aql were obtained starting 9 days after peak brightness and continued for 10 days. We were able to resolve the milliarcsecond-scale emission and follow the expansion of the nova photosphere. When combined with radial-velocity information, these observations can be used to infer the distance to the nova. Finally we have resolved the recurrent nova RS Oph and can draw some preliminary conclusions regarding the emission morphology.
• {Eisner}, J., , J. (2006). "{Massive Protoplanetary Disks in the Trapezium Region}". apj, 641, 1162-1171.
• {Eisner}, J., {Chiang}, E., , L. (2006). "{Spatially Resolving the Inner Disk of TW Hydrae}". apjl, 637, L133-L136.
• Akeson, R. L., Walker, C. H., Wood, K., Eisner, J. A., Scire, E., Penprase, B., Ciardi, D. R., Belle, G. V., Whitney, B., & Bjorkman, J. E. (2005). Observations and modeling of the inner disk region of T Tauri stars. Astrophysical Journal Letters, 622(1 I), 440-450.
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  Abstract: We present observations of four T Tauri stars using long baseline infrared interferometry from the Palomar Testbed Interferometer. The target sources, T Tau N, SU Aur, RY Tau, and DR Tau, are all known to be surrounded by dusty circumstellar disks. The observations directly trace the inner regions (
• Corder, S., Eisner, J., & Sargent, A. (2005). AB Aurigae resolved: Evidence for spiral structure. Astrophysical Journal Letters, 622(2 II), L133-L136.
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  Abstract: We have obtained high angular resolution (∼2″) images of the 13CO (J = 1 → 0) line and 2.7 mm continuum emission and slightly lower resolution images of 12CO (J→ 0) and C18O (J = 1 → 0) line emission toward the Herbig Ae star AB Aurigae. We resolve a circumstellar disk of diameter 780 AU (FWHM) with a velocity pattern consistent with a purely rotational disk at inclination 21°.5 and position angle 58°.6. Using Keplerian disk models, we find a central-source dynamical mass of 2.8 ±0.1 M⊙ and a cutoff radius of 615 AU for the 13CO emission. The inclination, mass, and radius determined from 12CO and C18O observations agree with these values, given optical depth and abundance effects. As a result of the high angular resolution of our observations, we confirm the existence of spiral structure suggested by near-infrared scattered-light images and show that the spiral arms represent density contrasts in the disk. © 2005. The American Astronomical Society. All rights reserved.
• Eisner, J. A., Hillenbrand, L. A., Carpenter, J. M., & Wolf, S. (2005). Constraining the evolutionary stage of Class I protostars: Multiwavelength observations and modeling. Astrophysical Journal Letters, 635(1 I), 396-421.
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  Abstract: We present new Keck images at 0.9 μm and OVRO 1.3 mm continuum images of five Class I protostars in the Taurus star-forming region. We analyze these data in conjunction with broadband spectral energy distributions (SEDs) and 8-13 μm spectra from the literature using a Monte Carlo radiative transfer code. By fitting models for the circumstellar dust distributions simultaneously to the scattered light images, millimeter continuum data, and the SEDs, we attempt to distinguish between flared disks, infalling envelopes with outflow cavities, and combinations of disks and envelopes. For each of these circumstellar density distributions, we generate grids of models for varying geometries, dust masses, and accretion rates and determine the best fits by minimizing the residuals between model and data. Comparison of the residuals for best-fit disk, envelope, and disk+envelope models demonstrates that, in general, models incorporating both massive envelopes and massive embedded disks fit the imaging+SED data best. The implied envelope infall rates for these disk+envelope models are generally consistent with infall rates derived by previous investigators, although they are approximately an order of magnitude larger than inner disk accretion rates inferred from recent spectroscopic measurements. In addition, the disk masses inferred from our models are close to or larger than the limit for gravitationally stable disks, indicating that Class I disks may undergo periodic episodes of enhanced accretion, perhaps as a result of gravitational instabilities. An important caveat to these results is that in some cases, no single model can fit all of the imaging and SED data well, suggesting that further refinements to models of the circumstellar dust distributions around Class I sources are necessary. We discuss several potential improvements to the models, as well as new constraints that will become available with upcoming millimeter and infrared facilities. © 2005. The American Astronomical Society. All rights reserved.
• Eisner, J. A., Hillenbrand, L. A., White, R. J., Akeson, R. L., & Sargent, A. I. (2005). Observations of T Tauri disks at sub-au radii: Implications for magnetospheric accretion and planet formation. Astrophysical Journal Letters, 623(2 I), 952-966.
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  Abstract: We determine inner disk sizes and temperatures for four solar-type (1-2 M⊙) classical T Tauri stars, AS 207A, V2508 Oph, AS 205A, and PX Vul, using 2.2 μm observations from the Keck Interferometer. Nearly contemporaneous near-IR adaptive optics imaging photometry, optical photometry, and high-dispersion optical spectroscopy are used to distinguish contributions from the inner disks and central stars in the interferometric observations. In addition, the spectroscopic and photometric data provide estimates of stellar properties, mass accretion rates, and disk corotation radii. We model our interferometric and photometric data in the context of geometrically flat accretion disk models with inner holes, and flared disks with puffed-up inner walls. Models incorporating puffed-up inner disk walls generally provide better fits to the data, similar to previous results for higher mass Herbig Ae stars. Our measured inner disk sizes are larger than disk truncation radii predicted by magnetospheric accretion models, with larger discrepancies for sources with higher mass accretion rates. We suggest that our measured sizes correspond to dust sublimation radii, and that optically thin gaseous material may extend farther inward to the magnetospheric truncation radii. Finally, our inner disk measurements constrain the location of terrestrial planet formation as well as potential mechanisms for halting giant planet migration. © 2005. The American Astronomical Society. All rights reserved.
• Lane, B. F., Retter, A., Thompson, R. R., & Eisner, J. A. (2005). Interferometric observations of V838 monocerotis. Astrophysical Journal Letters, 622(2 II), L137-L140.
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  Abstract: We have used long-baseline near-IR interferometry to resolve the peculiar eruptive variable star V838 Mon and to provide the first direct measurement of its angular size. Assuming a uniform disk model for the emission, we derive an apparent angular diameter at the time of observations (2004 November-December) of 1.83 ± 0.06 mas. For a nominal distance of 8 ± 2 kpc, this implies a linear radius of 1570 ± 400 R⊙. However, the data are somewhat better fitted by elliptical disk or binary component models, and we suggest that the emission may be strongly affected by ejecta from the outburst. © 2005. The American Astronomical Society. All rights reserved.
• Malbet, F., Lachaume, R., Berger, J. -., Colavita, M. M., Folco, E. D., Eisner, J. A., Lane, B. F., Millan-Gabet, R., Ségransan, D., & Traub, W. A. (2005). New insights on the AU-scale circumstellar structure of FU Orionis. Astronomy and Astrophysics, 437(2), 627-636.
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  Abstract: We report new near-infrared, long-baseline interferometric observations at the AU scale of the pre-main-sequence star FU Orionis with the PTI, IOTA and VLTI interferometers. This young stellar object has been observed on 42 nights over a period of 6 years from 1998 to 2003. We have obtained 287 independent measurements of the fringe visibility with 6 different baselines ranging from 20 to 110 m in length, in the H and K bands. Our data resolves FU Ori at the AU scale, and provides new constraints at shorter baselines and shorter wavelengths. Our extensive (u, v)-plane coverage, coupled with the published spectral energy distribution data, allows us to test the accretion disk scenario. We find that the most probable explanation for these observations is that FU Ori hosts an active accretion disk whose temperature law is consistent with standard models and with an accretion rate of M = (6.3±0.6) × 10 -5 (M*/M ⊙) -1 M ⊙ yr -1. We are able to constrain the geometry of the disk, including an inclination of 55 -7+5 deg and a position angle of 47 -11+7 deg. In addition, a 10 percent peak-to-peak oscillation is detected in the data (at the two-sigma level) from the longest baselines, which we interpret as a possible disk hot-spot or companion. The still somewhat limited (u, v) sampling and substantial measurement uncertainty prevent us from constraining the location of the spot with confidence, since many solutions yield a statistically acceptable fit. However, the oscillation in our best data set is best explained with an unresolved spot located at a projected distance of 10 ± 1 AU at the 130 ± 1 deg position angle and with a magnitude difference of ΔK ≈ 3.9 ± 0.2 and ΔH ≈ 3.6 ± 0.2 mag moving away from the center at a rate of 1.2 ± 0.6 AU yr -1. Although this bright spot on the surface of the disk could be tracing some thermal instabilities in the disk, we propose to interpret this spot as the signature of a companion of the central FU Ori system on an extremely eccentric orbit. We speculate that the close encounter of this putative companion and the central star could be the explanation of the initial photometric rise of the luminosity of this object. © ESO 2005.
• Metchev, S. A., Eisner, J. A., Hillenbrand, L. A., & Wolf, S. (2005). Adaptive optics imaging of the AU Microscopii circumstellar disk: Evidence for dynamical evolution. Astrophysical Journal Letters, 622(1 I), 451-462.
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  Abstract: We present an H-band image of the light scattered from circumstellar dust around the nearby (10 pc) young M star AU Microscopii (AU Mic, GJ 803, HD 197481), obtained with the Keck adaptive optics system. We resolve the disk both vertically and radially, tracing it over 17-60 AU from the star. Our high angular resolution (0.04 or 0.4 AU per resolution element) observations thus offer the opportunity to probe the morphology of the AU Mie debris disk on solar system scales. We identify substructures (dust clumps and gaps) in the disk that may point to the existence of orbiting planets. No planets are seen in our H-band image down to a limiting mass of 1MJ at >20 AU, although the existence of smaller planets cannot be excluded from the current data. Modeling of the disk surface brightness distribution at H band and R band, and of the optical to submillimeter spectral energy distribution, allows us to constrain the disk geometry and the dust grain properties. We confirm the nearly edge-on orientation of the disk inferred from previous observations and deduce that the disk may be clear inward of 1 -10 AU. We find evidence for a lack of small grains at
• {Akeson}, R., {Walker}, C., {Wood}, K., {Eisner}, J., {Scire}, E., {Penprase}, B., {Ciardi}, D., {van Belle}, G., {Whitney}, B., , J. (2005). "{Observations and Modeling of the Inner Disk Region of T Tauri Stars}". apj, 622, 440-450.
• {Corder}, S., {Eisner}, J., , A. (2005). "{AB Aurigae Resolved: Evidence for Spiral Structure}". apjl, 622, L133-L136.
• {Eisner}, J., {Hillenbrand}, L., {Carpenter}, J., , S. (2005). "{Constraining the Evolutionary Stage of Class I Protostars: Multiwavelength Observations and Modeling}". apj, 635, 396-421.
• {Eisner}, J., {Hillenbrand}, L., {White}, R., {Akeson}, R., , A. (2005). "{Observations of T Tauri Disks at Sub-AU Radii: Implications for Magnetospheric Accretion and Planet Formation}". apj, 623, 952-966.
• {Lane}, B., {Retter}, A., {Thompson}, R., , J. (2005). "{Interferometric Observations of V838 Monocerotis}". apjl, 622, L137-L140.
• {Malbet}, F., {Lachaume}, R., {Berger}, J., {Colavita}, M., {di Folco}, E., {Eisner}, J., {Lane}, B., {Millan-Gabet}, R., {S{'e}gransan}, D., , W. (2005). "{New insights on the AU-scale circumstellar structure of FU Orionis}". aap, 437, 627-636.
• {Metchev}, S., {Eisner}, J., {Hillenbrand}, L., , S. (2005). "{Adaptive Optics Imaging of the AU Microscopii Circumstellar Disk: Evidence for Dynamical Evolution}". apj, 622, 451-462.
• Eisner, J. A., Lane, B. F., Hillenbrand, L. A., Akeson, R. L., & Sargent, A. I. (2004). Resolved inner disks around Herbig Ae/Be stars. Astrophysical Journal Letters, 613(2 I), 1049-1071.
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  Abstract: We have observed 14 Herbig Ae/Be (HAEBE) sources with the long-baseline near-IR Palomar Testbed Interferometer. All except two sources are resolved at 2.2 μm, with angular sizes generally ≲ 5 mas. We determine the size scales and orientations of the 2.2 μm emission using various models: uniform disks, Gaussians, uniform rings, flat accretion disks with inner holes, and flared disks with puffed-up inner rims. Although it is difficult to distinguish different radial distributions, we are able to place firm constraints on the inclinations of most sources; seven objects display significantly inclined morphologies. The inner disk inclinations derived from our near-IR data are generally compatible with the outer disk geometries inferred from millimeter interferometric observations, implying that HAEBE disks are not significantly warped. Using the derived inner disk sizes and inclinations, we compute the spectral energy distributions (SEDs) for two simple physical disk models and compare these with observed SEDs compiled from the literature and new near-IR photometry. While geometrically flat accretion disk models are consistent with the data for the earliest spectral types in our sample (MWC 297, V1685 Cyg, and MWC 1080), the later type sources are explained better through models incorporating puffed-up inner disk walls. The different inner disk geometries may indicate different accretion mechanisms for early- and late-type HAEBE stars.
• {Eisner}, J., {Lane}, B., {Hillenbrand}, L., {Akeson}, R., , A. (2004). "{Resolved Inner Disks around Herbig Ae/Be Stars}". apj, 613, 1049-1071.
• Eisner, J. A., & Carpenter, J. M. (2003). Distribution of circumstellar disk masses in the young cluster NGC 2024. Astrophysical Journal Letters, 598(2 I), 1341-1349.
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  Abstract: We determine the distribution of circumstellar disk masses in the young (∼0.3 Myr) cluster NGC 2024 by imaging a 2′.5 × 2′.5 region in 3 mm continuum emission to an rms noise level of ∼0.75 mJy beam-1 with the Owens Valley Millimeter Array. The mosaic encompasses 147 K-band sources, as well as the molecular ridge seen previously in dust continuum emission. We detect 10 pointlike sources in 3 mm continuum emission above the level of 5 σ within the unit gain region of the mosaic. One of these sources corresponds to the near-IR source IRS 2, an early B-type star. Two other sources are tentatively associated with low-mass near-IR cluster members, and the remaining seven sources have no K-band counterparts. Assuming the millimeter continuum point sources represent emission from circumstellar disks and/or envelopes, then ∼6% of the total population (infrared and millimeter sources) in the NGC 2024 mosaic have a circumstellar mass in excess of ∼0.06 M⊙. We obtain further constraints on the average circumstellar disk mass by considering the mean millimeter continuum flux observed toward a sample of 140 K-band sources that likely have stellar masses ≲ 1-2 M⊙. While none of these sources are detected individually above the 3 σ limit of ∼0.035 M ⊙, the ensemble of sources are detected in the mean at the 5 σ level with a mean disk mass of ∼0.005 M⊙, Compared with the older (∼2 Myr) cluster IC 348, NGC 2024 contains a higher frequency of massive disks or envelopes and has a higher mean disk mass by a factor of 2.5 ± 1.3 among K-band sources, suggesting that the mean circumstellar mass is decreasing with cluster age. We also compare the results for the NGC 2024 and IC 348 clusters with those for the lower density Taurus star-forming region. Finally, we compare our detection limits with the minimum mass estimate for the proto-solar nebula and discuss possible implications for planet formation.
• Eisner, J. A., Lane, B. F., Akeson, R. L., Hillenbrand, L. A., & Sargent, A. I. (2003). Near-infrared interferometric measurements of herbig Ae/Be stars. Astrophysical Journal Letters, 588(1 I), 360-372.
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  Abstract: We have observed the Herbig Ae/Be sources AB Aur, VV Ser, V1685 Cyg (BD +40°4124), AS 442, and MWC 1080 with the Palomar Testbed Interferometer, obtaining the longest baseline near-IR interferometric observations of this class of objects. All of the sources are resolved at 2.2 μm with angular size scales generally ≲5 mas, consistent with the only previous near-IR interferometric measurements of Herbig Ae/Be stars, by Millan-Gabet and collaborators. We determine the angular size scales and orientations predicted by uniform-disk, Gaussian, ring, and accretion disk models. Although it is difficult to distinguish different radial distributions, we are able to place firm constraints on the inclinations of these models, and our measurements are the first that show evidence for significantly inclined morphologies. In addition, the derived angular sizes for the early-type Herbig Be stars in our sample, V1685 Cyg and MWC 1080, agree reasonably well with those predicted by the face-on accretion disk models used by Hillenbrand and collaborators to explain observed spectral energy distributions. In contrast, our data for the later-type sources AB Aur, VV Ser, and AS 442 are somewhat inconsistent with these models and may be explained better through the puffed-up inner disk models of Dullemond and collaborators.
• {Eisner}, J., , J. (2003). "{Distribution of Circumstellar Disk Masses in the Young Cluster NGC 2024}". apj, 598, 1341-1349.
• {Eisner}, J., {Lane}, B., {Akeson}, R., {Hillenbrand}, L., , A. (2003). "{Near-Infrared Interferometric Measurements of Herbig Ae/Be Stars}". apj, 588, 360-372.
• Eisner, J. A., & Kulkarni, S. R. (2002). Detecting outer planets in edge-on orbits: Combining radial velocity and astrometric techniques. Astrophysical Journal Letters, 574(1 I), 426-429.
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  Abstract: The astrometric and radial velocity techniques of extrasolar planet detection attempt to detect the periodic reflex motion of the parent star by extracting this periodic signal from a time-sampled set of observations. The extraction is generally accomplished using periodogram analysis or the functionally equivalent technique of least-squares fitting of sinusoids. In this paper, we use a frequentist approach to examine the sensitivity of the least-squares technique when applied to a combination of radial velocity and astrometric observations. We derive an analytical expression for the sensitivity and show that the combined approach yields significantly better sensitivity than either technique on its own. We discuss the ramifications of this result to upcoming astrometric surveys with the Full-Sky Astrometric Mapping Explorer, the Keck Interferometer, and the Space Interferometry Mission.
• Eisner, J. A., Greenhill, L. J., Herrnstein, J. R., Moran, J. M., & Menten, K. M. (2002). Outflow 20-2000 AU from a high-mass protostar in W51-IRS 2. Astrophysical Journal Letters, 569(1 I), 334-342.
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  Abstract: We present the results of the first high angular resolution observations of SiO maser emission toward the star-forming region W51-IRS 2 made with the Very Large Array (VLA) and Very Long Baseline Array (VLBA). Our images of the H2O maser emission in W51-IRS 2 reveal two maser complexes bracketing the SiO maser source. One of these H2O maser complexes appears to trace a bow shock whose opening angle is consistent with the opening angle observed in the distribution of SiO maser emission. A comparison of our H2O maser image with an image constructed from data acquired 19 years earlier clearly shows the persistence and motion of this bow shock. The proper motions correspond to an outflow velocity of 80 km s-1, which is consistent with the data of 19 years ago (that spanned 2 years). We have discovered a two-armed linear structure in the SiO maser emission on scales of ∼25 AU, and we find a velocity gradient on the order of 0.1 km s -1 AU-1 along the arms. We propose that the SiO maser source traces the limbs of an accelerating bipolar outflow close to an obscured protostar. We estimate that the outflow makes an angle of less than 20° with respect to the plane of the sky. Our measurement of the acceleration is consistent with a reported drift in the line-of-sight velocity of the W51 SiO maser source.
• {Eisner}, J., , S. (2002). "{Detecting Outer Planets in Edge-on Orbits: Combining Radial Velocity and Astrometric Techniques}". apj, 574, 426-429.
• {Eisner}, J., {Greenhill}, L., {Herrnstein}, J., {Moran}, J., , K. (2002). "{Outflow 20-2000 AU from a High-Mass Protostar in W51-IRS 2}". apj, 569, 334-342.
• Eisner, J. A., & Kulkarni, S. R. (2001). Sensitivity of the astrometric technique in detecting outer planets. Astrophysical Journal Letters, 561(2 PART 1), 1107-1115.
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  Abstract: With the advent of optical interferometers that will be coming on line in the next decade, radial velocity searches for extrasolar planets will be complemented by high angular resolution astrometric measurements. In this paper, we explore the sensitivity of the astrometric technique, and develop an analytical understanding of the sensitivity in the regime where the orbital period is longer than the time baseline of the survey. As in an earlier paper that dealt with the radial velocity technique, our analysis of the astrometric technique utilizes both the orbital amplitude and phase.
• Eisner, J. A., & Kulkarni, S. R. (2001). Sensitivity of the radial-velocity technique in detecting outer planets. Astrophysical Journal Letters, 550(2 PART 1), 871-883.
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  Abstract: The technique of measuring radial velocity (RV) has produced spectacular discoveries of short-period Jovian mass objects around a fraction (5%-10%) of nearby G stars. Although we expect Jovian planets to be located in long-period orbits of decades or longer (if our solar system is any guide), detecting such planets with the RV technique is difficult because of the smaller velocity amplitudes and the limited temporal baseline (5-10 yr) of current searches relative to the expected orbital periods. This paper develops an analytical understanding of the sensitivity of the RV technique in the regime in which the orbital period is larger than the total baseline of the survey. Moreover, we focus on the importance of the orbital phase in this "long-period" regime and develop a least-squares detection technique based on the amplitude and phase of the fitted signal. To illustrate the benefits of this amplitude-phase analysis, we compare it with existing techniques. Previous authors, such as Nelson and Angel in 1998, have explored the sensitivity of an amplitude-only analysis using Monte Carlo simulations. Others have supplemented this by using the slope of the linear component of the fitted sinusoid in addition (e.g., Walker and colleagues in 1995 and Cumming and colleagues in 1999). In this paper, we illustrate the benefits of the least-squares technique over periodogram analysis and demonstrate the superiority of an amplitude-phase technique over previous analyses.
• {Eisner}, J., , S. (2001). "{Sensitivity of the Astrometric Technique in Detecting Outer Planets}". apj, 561, 1107-1115.
• {Eisner}, J., , S. (2001). "{Sensitivity of the Radial-Velocity Technique in Detecting Outer Planets}". apj, 550, 871-883.
• {Kaplan}, D., {Eisner}, J., {Kulkarni}, S., , J. (2001). "{GRB 00630: Host Galaxy}". GRB Coordinates Network, 1069.

Proceedings Publications

• Eisner, J. (2021, mar). "ELT Imaging of Protoplanetary Disks and, Eventually, Protoplanets". In Bulletin of the American Astronomical Society, 53.
• Sallum, S., Skemer, A., Stelter, D., Briesemeister, Z., Batalha, N., Batalha, N., Blake, G., Brandt, T., Deich, W., Kleer, K., Pater, I., Eisner, J., Fitzgerald, M., Fong, W., Gerard, B., Greathouse, T., Greene, T., Hinz, P., Honda, M., , Jensen-Clem, R. .., et al. (2021, mar). "SCALES: Instrument Overview and Expected Science Outcomes". In 52nd Lunar and Planetary Science Conference.
• Anugu, N., Morzinski, K. M., Eisner, J., Douglas, E., Marrone, D., Ertel, S., Haffert, S., Montoya, O., Stone, J., Kraus, S., Monnier, J., Lebouquin, J., Berger, J., Woillez, J., & Montarg{`es}, M. (2020, aug). "Betelgeuse scope: single-mode-fibers-assisted optical interferometer design for dedicated stellar activity monitoring". In Interferometry XX, 11490.
• Boyden, R., & Eisner, J. (2020, feb). "Protoplanetary Disks in the Orion Nebula Cluster: Gas Disk Morphologies and Kinematics as seen with ALMA". In The 35th Annual New Mexico Symposium.
• Sallum, S., Skemer, A., Eisner, J., Marel, N., Sheehan, P., Close, L., Ireland, M., Males, J., Morzinski, K., Bailey, V., Briguglio, R., & Puglisi, A. (2019, Aug). New Spatially Resolved Observations of the SR 21 Transition Disk. In AAS/Division for Extreme Solar Systems Abstracts, 51.
• Kim, J., Fang, M., Eisner, J., Pascucci, I., Apai, D., Clarke, C., Facchini, S., Manara, C., Kounkel, M., & Covey, K. (2018, jul). Probing Effect of External UV Radiation on Young Stellar and Substellar Mass Objects: Is Orion a Special Place for Observing External Photoevaporation of Disks?. In 20th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.
• Sivanandam, S., Moon, D., Meyer, R., Grunhut, J., Zaritsky, D., Eisner, J., Ma, K., Henderson, C., Blank, B., Chou, C., Jarvis, M., Eikenberry, S., Chun, M., & Park, B. (2018, jul). The wide integral field infrared spectrograph: commissioning results and on-sky performance. In Ground-based and Airborne Instrumentation for Astronomy VII, 10702.
• Sheehan, P., & Eisner, J. (2017, jan). "Disk Masses of Class I Protostars in Taurus and Ophiuchus". In American Astronomical Society Meeting Abstracts #229, 229.
• Crepp, J., Crass, J., King, D., Bechter, A., Bechter, E., Ketterer, R., Reynolds, R., Hinz, P., Kopon, D., Cavalieri, D., Fantano, L., Koca, C., Onuma, E., Stapelfeldt, K., Thomes, J., Wall, S., Macenka, S., McGuire, J., Korniski, R., , Zugby, L., et al. (2016, aug). "iLocater: a diffraction-limited Doppler spectrometer for the Large Binocular Telescope". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 9908.
• Sallum, S., Eisner, J., Close, L., Hinz, P., Follette, K., Kratter, K., Skemer, A., Bailey, V., Briguglio, R., Defrere, D., Macintosh, B., Males, J., Morzinski, K., Puglisi, A., Rodigas, T., Spalding, E., Tuthill, P., Vaz, A., Weinberger, A., & Xomperio, M. (2016, aug). "Imaging protoplanets: observing transition disks with non-redundant masking". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 9907.
• {Follette}, K., {Miller Close}, L., {Males}, J., {Macintosh}, B., {Sallum}, S., {Eisner}, J., {Kratter}, K., {Bailey}, V., {Defrere}, D., {Hinz}, P., {Morzinski}, K., {Rodigas}, T., {Skemer}, A., {Spalding}, E., {Tuthill}, P., {Vaz}, A., , A. (2016, jan). "{An Accreting Protoplanet: Confirmation and Characterization of LkCa15b}". In American Astronomical Society Meeting Abstracts, 227.
• {Kuhn}, B., {Eisner}, J., , J. (2016, jan). "{Time Monitoring Variability of Classical Be Stars}". In American Astronomical Society Meeting Abstracts, 227.
• {Defr{`e}re}, D., {Hinz}, P., {Skemer}, A., {Bailey}, V., {Downey}, E., {Durney}, O., {Eisner}, J., {Hill}, J., {Hoffmann}, W., {Leisenring}, J., {McMahon}, T., {Montoya}, M., {Spalding}, E., {Stone}, J., {Vaz}, A., {Absil}, O., {Esposito}, S., {Kenworthy}, M., {Mennesson}, B., , {Millan-Gabet}, R., et al. (2015, sep). "{Exoplanet science with the LBTI: instrument status and plans}". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 9605.
• {Follette}, K., {Close}, L., {Males}, J., {Macintosh}, B., {Sallum}, S., {Eisner}, J., {Kratter}, K., {Morzinski}, K., {Hinz}, P., {Weinberger}, A., {Rodigas}, T., {Skemer}, A., {Bailey}, V., {Vaz}, A., {Defrere}, D., {spalding}, e., , P. (2015, dec). "An Accreting Protoplanet: Confirmation and Characterization of LkCa15b". In AAS/Division for Extreme Solar Systems Abstracts, 3.
• {Sivanandam}, S., {Moon}, D., {Zaritsky}, D., {Chou}, R., {Meyer}, E., {Ma}, K., {Jarvis}, M., , J. (2015, jan). "{Wide Integral Field Infrared Spectroscopic Survey of Nearby Galaxies}". In American Astronomical Society Meeting Abstracts, 225.
• Bechter, E., Bechter, A., Crepp, J. R., Berg, M., Carroll, J., Collins, K., Corpuz, T., Ketterer, R., Kielb, E., Stoddard, R., Eisner, J., Gaudi, B. S., Hinz, P., Kratter, K., Macela, G., Quirrenbach, A., Skrutskie, M., Sozzetti, A., Woodward, C. E., & Zhao, B. (2014, mar). The iLocater Doppler Spectrometer. In Search for Life Beyond the Solar System. Exoplanets, Biosignatures amp Instruments, 3P.
• Crepp, J. R., Bechter, A., Bechter, E., Berg, M., Carroll, J., Collins, K., Corpuz, T., Ketterer, R., Kielb, E., Stoddard, R., Eisner, J. A., Gaudi, B. S., Hinz, P., Kratter, K. M., Macela, G., Quirrenbach, A., Skrutskie, M. F., Sozzetti, A., Woodward, C. E., & Zhao, B. (2014, jan). iLocater: A Diffraction-Limited Doppler Spectrometer for the Large Binocular Telescope. In American Astronomical Society Meeting Abstracts, 223, #348.20.
• Defrere, D., Hinz, P., Skemer, A., Arbo, P., Bailey, V., Brusa, G., Connors, T., Downey, E., Durney, O., Eisner, J., Grenz, P., Hoffmann, B., Hill, J., Leisenring, J., McMahon, T., Mennesson, M., Millan-Gabet, R., Montoya, M., Nash, M., , Skrutskie, M., et al. (2014, apr). Update on the LBTI: a versatile high-contrast and high-resolution infrared imager for a 23-m telescope. In Improving the Performances of Current Optical Interferometers amp Future Designs, 37-44.
• Eisner, J. A. (2014, sep). The Inner AU of Protoplanetary Disks: From Visibilities to Spectra to Images. In Resolving The Future Of Astronomy With Long-Baseline Interferometry, 487, 65.
• Skemer, A. J., Hinz, P., Esposito, S., Skrutskie, M. F., Defr`ere, D., Bailey, V., Leisenring, J., Apai, D., Biller, B., Bonnefoy, M., Brandner, W., Buenzli, E., Close, L., Crepp, J., De Rosa, R. J., Desidera, S., Eisner, J., Fortney, J., Henning, T., , Hofmann, K., et al. (2014, jul). High contrast imaging at the LBT: the LEECH exoplanet imaging survey. In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 9148, 0.
• Skemer, A., Apai, D., Bailey, V., Biller, B., Bonnefoy, M., Brandner, W., Buenzli, E., Close, L., Crepp, J., Defrere, D., Desidera, S., Eisner, J., Esposito, S., Fortney, J., Henning, T., Hinz, P., Hofmann, K., Leisenring, J., Males, J., , Millan-Gabet, R., et al. (2014, jan). LEECH: A 100 Night Exoplanet Imaging Survey at the LBT. In IAU Symposium, 299, 70-71.
• {Bechter}, E., {Bechter}, A., {Crepp}, J., {Berg}, M., {Carroll}, J., {Collins}, K., {Corpuz}, T., {Ketterer}, R., {Kielb}, E., {Stoddard}, R., {Eisner}, J., {Gaudi}, B., {Hinz}, P., {Kratter}, K., {Macela}, G., {Quirrenbach}, A., {Skrutskie}, M., {Sozzetti}, A., {Woodward}, C., , B. (2014, mar). "{The iLocater Doppler Spectrometer}". In Search for Life Beyond the Solar System. Exoplanets, Biosignatures {amp} Instruments.
• {Crepp}, J., {Bechter}, A., {Bechter}, E., {Berg}, M., {Carroll}, J., {Collins}, K., {Corpuz}, T., {Ketterer}, R., {Kielb}, E., {Stoddard}, R., {Eisner}, J., {Gaudi}, B., {Hinz}, P., {Kratter}, K., {Macela}, G., {Quirrenbach}, A., {Skrutskie}, M., {Sozzetti}, A., {Woodward}, C., , B. (2014, jan). "{iLocater: A Diffraction-Limited Doppler Spectrometer for the Large Binocular Telescope}". In American Astronomical Society Meeting Abstracts #223, 223.
• {Defr{`e}re}, D., {Hinz}, P., {Skemer}, A., {Arbo}, P., {Bailey}, V., {Brusa}, G., {Connors}, T., {Downey}, E., {Durney}, O., {Eisner}, J., {Grenz}, P., {Hoffmann}, B., {Hill}, J., {Leisenring}, J., {McMahon}, T., {Mennesson}, M., {Millan-Gabet}, R., {Montoya}, M., {Nash}, M., , {Skrutskie}, M., et al. (2014, apr). "{Update on the LBTI: a versatile high-contrast and high-resolution infrared imager for a 23-m telescope}". In Improving the Performances of Current Optical Interferometers {amp} Future Designs.
• {Eisner}, J. (2014, sep). "{The Inner AU of Protoplanetary Disks: From Visibilities to Spectra to Images}". In Resolving The Future Of Astronomy With Long-Baseline Interferometry, 487.
• {Skemer}, A., {Apai}, D., {Bailey}, V., {Biller}, B., {Bonnefoy}, M., {Brandner}, W., {Buenzli}, E., {Close}, L., {Crepp}, J., {Defrere}, D., {Desidera}, S., {Eisner}, J., {Esposito}, S., {Fortney}, J., {Henning}, T., {Hinz}, P., {Hofmann}, K., {Leisenring}, J., {Males}, J., , {Millan-Gabet}, R., et al. (2014, jan). "{LEECH: A 100 Night Exoplanet Imaging Survey at the LBT}". In IAU Symposium, 299.
• {Skemer}, A., {Hinz}, P., {Esposito}, S., {Skrutskie}, M., {Defr{`e}re}, D., {Bailey}, V., {Leisenring}, J., {Apai}, D., {Biller}, B., {Bonnefoy}, M., {Brandner}, W., {Buenzli}, E., {Close}, L., {Crepp}, J., {De Rosa}, R., {Desidera}, S., {Eisner}, J., {Fortney}, J., {Henning}, T., , {Hofmann}, K., et al. (2014, jul). "{High contrast imaging at the LBT: the LEECH exoplanet imaging survey}". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 9148.
• Cole, A., Eisner, J. A., & Rudolph, A. L. (2013, jan). Near-IR Spectral Variability of Be Stars. In American Astronomical Society Meeting Abstracts, 221, #256.16.
• Zimmerman, N., Skemer, A., Apai, D., Bailey, V., Biller, B., Bonnefoy, M., Brandner, W., Buenzli, E., Close, L., Crepp, J., Defrere, D., Desidera, S., Eisner, J., Esposito, S., Fortney, J., Henning, T., Hinz, P., Hofmann, K., Leisenring, J., , Males, J., et al. (2013, jul). A 100-Night Exoplanet Imaging Survey at the LBT. In Protostars and Planets VI Posters, 6.
• {Cole}, A., {Eisner}, J., , A. (2013, jan). "{Near-IR Spectral Variability of Be Stars}". In American Astronomical Society Meeting Abstracts #221, 221.
• {Zimmerman}, N., {Skemer}, A., {Apai}, D., {Bailey}, V., {Biller}, B., {Bonnefoy}, M., {Brandner}, W., {Buenzli}, E., {Close}, L., {Crepp}, J., {Defrere}, D., {Desidera}, S., {Eisner}, J., {Esposito}, S., {Fortney}, J., {Henning}, T., {Hinz}, P., {Hofmann}, K., {Leisenring}, J., , {Males}, J., et al. (2013, jul). "{A 100-Night Exoplanet Imaging Survey at the LBT}". In Protostars and Planets VI Posters.
• Hawkins, C., Eisner, J., & Rudolph, A. L. (2012, jan). Near-IR Spectral Variability Of Young Stars: A Multi-year Survey. In American Astronomical Society Meeting Abstracts #219, 219, #344.03.
• {Hawkins}, C., {Eisner}, J., , A. (2012, jan). "{Near-IR Spectral Variability Of Young Stars: A Multi-year Survey}". In American Astronomical Society Meeting Abstracts #219, 219.
• {Leisenring}, J., {Skrutskie}, M., {Hinz}, P., {Skemer}, A., {Bailey}, V., {Eisner}, J., {Garnavich}, P., {Hoffmann}, W., {Jones}, T., {Kenworthy}, M., {Kuzmenko}, P., {Meyer}, M., {Nelson}, M., {Rodigas}, T., {Wilson}, J., , V. (2012, sep). "{On-sky operations and performance of LMIRcam at the Large Binocular Telescope}". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 8446.
• {Sivanandam}, S., {Chou}, R., {Moon}, D., {Ma}, K., {Millar-Blanchaer}, M., {Eikenberry}, S., {Chun}, M., {Kim}, S., {Raines}, S., , J. (2012, sep). "{The development of WIFIS: a wide integral field infrared spectrograph}". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 8446.
• {Woillez}, J., {Wizinowich}, P., {Akeson}, R., {Colavita}, M., {Eisner}, J., {Millan-Gabet}, R., {Monnier}, J., {Pott}, J., {Ragland}, S., {Appleby}, E., {Cooper}, A., {Felizardo}, C., {Herstein}, J., {Martin}, O., {Medeiros}, D., {Morrison}, D., {Panteleeva}, T., {Smith}, B., {Summers}, K., , {Tsubota}, K., et al. (2012, jul). "{First faint dual-field phase-referenced observations on the Keck interferometer}". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 8445.
• {Arnold}, T., , J. (2011, jan). "{Variability And Disk Geometry In The Classical T Tauri Star Tw Hya Using Mid-infrared Speckle Interferometry}". In American Astronomical Society Meeting Abstracts #217, 43.
• {Zajac}, S., {Eisner}, J., , A. (2011, jan). "{Near-IR Spectral Variability of Young Stars}". In American Astronomical Society Meeting Abstracts #217, 43.
• {Eisner}, J., {Akeson}, R., {Colavita}, M., {Ghez}, A., {Graham}, J., {Hillenbrand}, L., {Millan-Gabet}, R., {Monnier}, J., {Pott}, J., {Ragland}, S., {Wizinowich}, P., , J. (2010, jul). "{Science with the Keck Interferometer ASTRA program}". In Optical and Infrared Interferometry II, 7734.
• {Pott}, J., {Woillez}, J., {Ragland}, S., {Wizinowich}, P., {Eisner}, J., {Monnier}, J., {Akeson}, R., {Ghez}, A., {Graham}, J., {Hillenbrand}, L., {Millan-Gabet}, R., {Appleby}, E., {Berkey}, B., {Colavita}, M., {Cooper}, A., {Felizardo}, C., {Herstein}, J., {Hrynevych}, M., {Medeiros}, D., , {Morrison}, D., et al. (2010, jul). "{First Keck Interferometer measurements in self-phase referencing mode: spatially resolving circum-stellar line emission of 48 Lib}". In Optical and Infrared Interferometry II, 7734.
• {Woillez}, J., {Akeson}, R., {Colavita}, M., {Eisner}, J., {Ghez}, A., {Graham}, J., {Hillenbrand}, L., {Millan-Gabet}, R., {Monnier}, J., {Pott}, J., {Ragland}, S., {Wizinowich}, P., {Appleby}, E., {Berkey}, B., {Cooper}, A., {Felizardo}, C., {Herstein}, J., {Hrynevych}, M., {Martin}, O., , {Medeiros}, D., et al. (2010, jul). "{ASTRA: astrometry and phase-referencing astronomy on the Keck interferometer}". In Optical and Infrared Interferometry II, 7734.
• {Millan-Gabet}, R., {Monnier}, J., {Akeson}, R., {Beichman}, C., {brittain}, S., {ten Brummelaar}, T., {Calvet}, N., {Eisner}, J., {Hinz}, P., {Jang-Congell}, H., {Kuchner}, M., {Malbet}, F., {Matt}, S., {Najita}, J., {Raymond}, S., {Roberge}, A., {Tannirkulam}, A., {Turner}, N., , D. (2009). "{How and When Do Planets Form? The Inner Regions of Planet Forming Disks at High Spatial and Spectral Resolution}". In astro2010: The Astronomy and Astrophysics Decadal Survey, 2010.
• {Lane}, B., {Retter}, A., {Eisner}, J., {Thompson}, R., , M. (2006, jun). "{Interferometric observations of explosive variables: V838 Mon, Nova Aql 2005, and RS Oph}". In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 6268.
• {Eisner}, J., {Hillenbrand}, L., {Lane}, B., {Akeson}, R., {White}, R., , A. (2005). "{Probing Sub-AU Radii of Protoplanetary Disks with NIR Interferometry}". In Protostars and Planets V Posters, 1286.
• {Lane}, B., {Retter}, A., {Eisner}, J., {Thompson}, R., , M. (2005, dec). "{Interferometric Observations of Nova Aql 2005}". In American Astronomical Society Meeting Abstracts, 37.
• {Eisner}, J. (2004, dec). "{High Angular Resolution Studies of Young Circumstellar Disks}". In American Astronomical Society Meeting Abstracts, 36.
• {Eisner}, J., , B. (2002, dec). "{Near-IR Interferometric Observations of Herbig Ae/Be Stars}". In American Astronomical Society Meeting Abstracts, 34.
• {Eisner}, J., , S. (2001, may). "{Combining Astrometric and Radial Velocity Techniques for Detecting Outer Planets}". In American Astronomical Society Meeting Abstracts #198, 33.
• {Eisner}, J., {Herrnstein}, J., {Greenhill}, L., , K. (1998, dec). "{SiO Masers, Water Masers, and Outflow in the W51-IRS2 star-forming region}". In American Astronomical Society Meeting Abstracts, 30.

Presentations

• Kim, J. S., Pascucci, I., Apai, D., & Eisner, J. A. (2017, November). EARTHS IN OTHER SOLAR SYSTEMS: FUNDAMENTAL PROTOPLANETARY DISK PROPERTIES AND THEIR EVOLUTION. Habitable Worlds 2017: A System Science Workshop (NASA NExSS workshop). Laramie, WY: NASA - the Nexus for Exoplanet System Science (NExSS).
  More info

  The Nexus for Exoplanet System Science (NExSS), a NASA research coordination network dedicated to the study of planetary habitability held a five-day workshop on Habitable Worlds 2017: A System Science Workshop, November 13–17, 2017 at the University of Wyoming Conference Center (UWCC) and Marian H. Rochelle Gateway Center (MHRGC) in Laramie, Wyoming. I was one of the local organization committee and also served to select scientific programs.

Others

• {Eisner}, J. (2011). "{Imaging Sub-AU-Sized Regions of Protoplanetary Disks in the near-IR}".
• {Eisner}, J. (2010). "{Probing the Gas Content of Terrestrial and Giant Planet Forming Regions of Protoplanetary Disks}".
• {Eisner}, J., {Monnier}, J., {Espaillat}, C., , N. (2008). "{Resolving Large Inner Disk Clearings with TReCS}".
• {Eisner}, J. (2005). "{High angular resolution studies of the structure and evolution of protoplanetary disks}".