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1,126 results on '"Beichman, C."'

151. The HOSTS survey: evidence for an extended dust disk and constraints on the presence of giant planets in the Habitable Zone of $��$ Leo

Author

Defr��re, D., Hinz, P. M., Kennedy, G. M., Stone, J., Rigley, J., Ertel, S., Gaspar, A., Bailey, V. P., Hoffmann, W. F., Mennesson, B., Millan-Gabet, R., Danchi, W. C., Absil, O., Arbo, P., Beichman, C., Bonavita, M., Brusa, G., Bryden, G., Downey, E. C., Esposito, S., Grenz, P., Haniff, C., Hill, J. M., Leisenring, J. M., Males, J. R., McMahon, T. J., Montoya, M., Morzinski, K. M., Pinna, E., Puglisi, A., Rieke, G., Roberge, A., Rousseau, H., Serabyn, E., Spalding, E., Skemer, A. J., Stapelfeldt, K., Su, K., Vaz, A., Weinberger, A. J., and Wyatt, M. C.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The young (50-400 Myr) A3V star $��$ Leo is a primary target to study the formation history and evolution of extrasolar planetary systems as one of the few stars with known hot ($\sim$1600$^\circ$K), warm ($\sim$600$^\circ$K), and cold ($\sim$120$^\circ$K) dust belt components. In this paper, we present deep mid-infrared measurements of the warm dust brightness obtained with the Large Binocular Telescope Interferometer (LBTI) as part of its exozodiacal dust survey (HOSTS). The measured excess is 0.47\%$\pm$0.050\% within the central 1.5 au, rising to 0.81\%$\pm$0.026\% within 4.5 au, outside the habitable zone of $��$~Leo. This dust level is 50 $\pm$ 10 times greater than in the solar system's zodiacal cloud. Poynting-Robertson drag on the cold dust detected by Spitzer and Herschel under-predicts the dust present in the habitable zone of $��$~Leo, suggesting an additional delivery mechanism (e.g.,~comets) or an additional belt at $\sim$5.5 au. A model of these dust components is provided which implies the absence of planets more than a few Saturn masses between $\sim$5 au and the outer belt at $\sim$40 au. We also observationally constrain giant planets with the LBTI imaging channel at 3.8~$��$m wavelength. Assuming an age of 50 Myr, any planet in the system between approximately 5 au to 50 au must be less than a few Jupiter masses, consistent with our dust model. Taken together, these observations showcase the deep contrasts and detection capabilities attainable by the LBTI for both warm exozodiacal dust and giant exoplanets in or near the habitable zone of nearby stars., 11 pages, 9 figures, accepted for publication in Astronomical Journal

Published
2021
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152. Extreme Precision Radial Velocity Working Group Final Report

Author

Crass, J., Gaudi, B. Scott, Leifer, S., Beichman, C. A., Bender, Chad, Blackwood, Gary, Burt, Jennifer A., Callas, John L., Cegla, Heather M., Diddams, Scott A., Dumusque, Xavier, Eastman, Jason D., Ford, Eric B., Fulton, B. J., Gibson, Rose, Halverson, Samuel, Haywood, Raphaëlle D., Hearty, Fred, Howard, A., Latham, David W., Löhner-Böttcher, Johannes, Mamajek, Eric E., Mortier, Annelies, Newman, Patrick, Plavchan, Peter, Quirrenbach, Andreas, Reiners, Ansgar, Robertson, Paul, Roy, Arpita, Schwab, Christian, Seifahrt, Andres, Szentgyorgyi, Andy, Terrien, Ryan, Teske, Johanna K., Thompson, Samantha, Vasisht, G., Crass, J., Gaudi, B. Scott, Leifer, S., Beichman, C. A., Bender, Chad, Blackwood, Gary, Burt, Jennifer A., Callas, John L., Cegla, Heather M., Diddams, Scott A., Dumusque, Xavier, Eastman, Jason D., Ford, Eric B., Fulton, B. J., Gibson, Rose, Halverson, Samuel, Haywood, Raphaëlle D., Hearty, Fred, Howard, A., Latham, David W., Löhner-Böttcher, Johannes, Mamajek, Eric E., Mortier, Annelies, Newman, Patrick, Plavchan, Peter, Quirrenbach, Andreas, Reiners, Ansgar, Robertson, Paul, Roy, Arpita, Schwab, Christian, Seifahrt, Andres, Szentgyorgyi, Andy, Terrien, Ryan, Teske, Johanna K., Thompson, Samantha, and Vasisht, G.

Abstract

Precise mass measurements of exoplanets discovered by the direct imaging or transit technique are required to determine planet bulk properties and potential habitability. Furthermore, it is generally acknowledged that, for the foreseeable future, the Extreme Precision Radial Velocity (EPRV) measurement technique is the only method potentially capable of detecting and measuring the masses and orbits of habitable-zone Earths orbiting nearby F, G, and K spectral-type stars from the ground. In particular, EPRV measurements with a precision of better than approximately 10 cm/s (with a few cm/s stability over many years) are required. Unfortunately, for nearly a decade, PRV instruments and surveys have been unable to routinely reach RV accuracies of less than roughly 1 m/s. Making EPRV science and technology development a critical component of both NASA and NSF program plans is crucial for reaching the goal of detecting potentially habitable Earthlike planets and supporting potential future exoplanet direct imaging missions such as the Habitable Exoplanet Observatory (HabEx) or the Large Ultraviolet Optical Infrared Surveyor (LUVOIR). In recognition of these facts, the 2018 National Academy of Sciences (NAS) Exoplanet Science Strategy (ESS) report recommended the development of EPRV measurements as a critical step toward the detection and characterization of habitable, Earth-analog planets. In response to the NAS-ESS recommendation, NASA and NSF commissioned the EPRV Working Group to recommend a ground-based program architecture and implementation plan to achieve the goal intended by the NAS. This report documents the activities, findings, and recommendations of the EPRV Working Group.

Published
2021

153. The HOSTS Survey: Evidence for an Extended Dust Disk and Constraints on the Presence of Giant Planets in the Habitable Zone of β Leo

Author

Defrère, D., primary, Hinz, P. M., additional, Kennedy, G. M., additional, Stone, J., additional, Rigley, J., additional, Ertel, S., additional, Gaspar, A., additional, Bailey, V. P., additional, Hoffmann, W. F., additional, Mennesson, B., additional, Millan-Gabet, R., additional, Danchi, W. C., additional, Absil, O., additional, Arbo, P., additional, Beichman, C, additional, Bonavita, M, additional, Brusa, G., additional, Bryden, G., additional, Downey, E. C., additional, Esposito, S., additional, Grenz, P., additional, Haniff, C., additional, Hill, J. M., additional, Leisenring, J. M., additional, Males, J. R., additional, McMahon, T. J., additional, Montoya, M., additional, Morzinski, K. M., additional, Pinna, E., additional, Puglisi, A., additional, Rieke, G., additional, Roberge, A., additional, Rousseau, H., additional, Serabyn, E., additional, Spalding, E., additional, Skemer, A. J., additional, Stapelfeldt, K., additional, Su, K., additional, Vaz, A., additional, Weinberger, A. J., additional, and Wyatt, M. C., additional

Published
2021
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154. The HOSTS Survey for Exozodiacal Dust: Observational Results from the Complete Survey

Author

Stone, J. M., Ertel, S, Defrere, D, Hinz, P, Mennesson, B, Kennedy, GM, Danchi, WC, Gelino, C, Hill, JM, Hoffmann, WF, Mazoyer, J, Rieke, G, Shannon, A, Stapelfeldt, K, Spalding, E, Stone, JM, Vaz, A, Weinberger, AJ, Willems, P, Absil, O, Arbo, P, Bailey, VP, Beichman, C, Bryden, G, Downey, EC, Durney, O, Esposito, S, Gaspar, A, Grenz, P, Haniff, CA, Leisenring, JM, Marion, L, McMahon, TJ, Millan-Gabet, R, Montoya, M, Morzinski, KM, Perera, S, Pinna, E, Pott, JU, Power, J, Puglisi, A, Roberge, A, Serabyn, E, Skemer, AJ, Su, KYL, Vaitheeswaran, V, Wyatt, MC, J. M. Stone [0000-0003-0454-3718], Ertel, S [0000-0002-2314-7289], Mennesson, B [0000-0003-4205-4800], Mazoyer, J [0000-0002-9133-3091], Rieke, G [0000-0003-2303-6519], Shannon, A [0000-0002-0711-4516], Stapelfeldt, K [0000-0002-2805-7338], Weinberger, AJ [0000-0001-6654-7859], Absil, O [0000-0002-4006-6237], Bailey, VP [0000-0002-5407-2806], Gaspar, A [0000-0001-8612-3236], Leisenring, JM [0000-0002-0834-6140], Millan-Gabet, R [0000-0003-0447-5866], Morzinski, KM [0000-0002-1384-0063], Pott, JU [0000-0003-4291-2078], Roberge, A [0000-0002-2989-3725], Skemer, AJ [0000-0001-6098-3924], Su, KYL [0000-0002-3532-5580], Wyatt, MC [0000-0001-9064-5598], and Apollo - University of Cambridge Repository

Subjects
Habitable zone, Debris disks, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Exozodiacal dust, Habitable planets, Astrophysics::Galaxy Astrophysics
Abstract

The Large Binocular Telescope Interferometer (LBTI) enables nulling interferometric observations across the N band (8 to 13 um) to suppress a star's bright light and probe for faint circumstellar emission. We present and statistically analyze the results from the LBTI/HOSTS (Hunt for Observable Signatures of Terrestrial Systems) survey for exozodiacal dust. By comparing our measurements to model predictions based on the Solar zodiacal dust in the N band, we estimate a 1 sigma median sensitivity of 23 zodis for early type stars and 48 zodis for Sun-like stars, where 1 zodi is the surface density of habitable zone (HZ) dust in the Solar system. Of the 38 stars observed, 10 show significant excess. A clear correlation of our detections with the presence of cold dust in the systems was found, but none with the stellar spectral type or age. The majority of Sun-like stars have relatively low HZ dust levels (best-fit median: 3 zodis, 1 sigma upper limit: 9 zodis, 95% confidence: 27 zodis based on our N band measurements), while ~20% are significantly more dusty. The Solar system's HZ dust content is consistent with being typical. Our median HZ dust level would not be a major limitation to the direct imaging search for Earth-like exoplanets, but more precise constraints are still required, in particular to evaluate the impact of exozodiacal dust for the spectroscopic characterization of imaged exo-Earth candidates.

Published
2020
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155. Toi-1235 b: A keystone super-earth for testing radius valley emergence models around early m dwarfs

Author

Cloutier, R, Rodriguez, JE, Irwin, J, Charbonneau, D, Stassun, KG, Mortier, A, Latham, DW, Isaacson, H, Howard, AW, Udry, S, Wilson, TG, Watson, CA, Pinamonti, M, Lienhard, F, Giacobbe, P, Guerra, P, Collins, KA, Beiryla, A, Esquerdo, GA, Matthews, E, Matson, RA, Howell, SB, Furlan, E, Crossfield, IJM, Winters, JG, Nava, C, Ment, K, Lopez, ED, Ricker, G, Vanderspek, R, Seager, S, Jenkins, JM, Ting, EB, Tenenbaum, P, Sozzetti, A, Sha, L, Ségransan, D, Schlieder, JE, Sasselov, D, Roy, A, Robertson, P, Rice, K, Poretti, E, Piotto, G, Phillips, D, Pepper, J, Pepe, F, Molinari, E, Mocnik, T, Micela, G, Mayor, M, Martinez Fiorenzano, AF, Mallia, F, Lubin, J, Lovis, C, López-Morales, M, Kosiarek, MR, Kielkopf, JF, Kane, Jensen, ELN, Isopi, G, Huber, D, Hill, ML, Harutyunyan, A, Gonzales, E, Giacalone, S, Ghedina, A, Ercolino, A, Dumusque, X, Dressing, CD, Damasso, M, Dalba, PA, Cosentino, R, Conti, DM, Colón, KD, Collins, KI, Cameron, AC, Ciardi, D, Christiansen, J, Chontos, A, Cecconi, M, Caldwell, DA, Burke, C, Buchhave, L, Beichman, C, Behmard, A, Beard, C, Akana Murphy, JM, Cloutier, R [0000-0001-5383-9393], Rodriguez, JE [0000-0001-8812-0565], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Mortier, A [0000-0001-7254-4363], Latham, DW [0000-0001-9911-7388], Isaacson, H [0000-0002-0531-1073], Howard, AW [0000-0001-8638-0320], Udry, S [0000-0001-7576-6236], Collins, KA [0000-0001-6588-9574], Beiryla, A [0000-0001-6637-5401], Esquerdo, GA [0000-0002-9789-5474], Matthews, E [0000-0003-0593-1560], Matson, RA [0000-0001-7233-7508], Howell, SB [0000-0002-2532-2853], Winters, JG [0000-0001-6031-9513], Nava, C [0000-0001-8838-3883], Ment, K [0000-0001-5847-9147], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Ting, EB [0000-0002-8219-9505], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Sha, L [0000-0001-5401-8079], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Roy, A [0000-0001-8127-5775], Robertson, P [0000-0003-0149-9678], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Pepper, J [0000-0002-3827-8417], Molinari, E [0000-0002-1742-7735], Mocnik, T [0000-0003-4603-556X], Micela, G [0000-0002-9900-4751], Lubin, J [0000-0001-8342-7736], López-Morales, M [0000-0003-3204-8183], Kielkopf, JF [0000-0003-0497-2651], Kane, SR [0000-0002-7084-0529], Jensen, ELN [0000-0002-4625-7333], Huber, D [0000-0001-8832-4488], Hill, ML [0000-0002-0139-4756], Giacalone, S [0000-0002-8965-3969], Ghedina, A [0000-0003-4702-5152], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Dalba, PA [0000-0002-4297-5506], Cosentino, R [0000-0003-1784-1431], Conti, DM [0000-0003-2239-0567], Colón, KD [0000-0001-8020-7121], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Christiansen, J [0000-0002-8035-4778], Chontos, A [0000-0003-1125-2564], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Behmard, A [0000-0003-0012-9093], Beard, C [0000-0001-7708-2364], Akana Murphy, JM [0000-0001-8898-8284], and Apollo - University of Cambridge Repository

Subjects
Radial velocity, Exoplanet formation, Transit photometry, M dwarf stars, Exoplanet structure
Abstract

Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally-driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/non-rocky transition in period-radius space. Here we present the confirmation of TOI-1235 b ($P=3.44$ days, $r_p=1.738^{+0.087}_{-0.076}$ R$_{\oplus}$), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/non-rocky transition around early M dwarfs ($R_s=0.630\pm 0.015$ R$_{\odot}$, $M_s=0.640\pm 0.016$ M$_{\odot}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial-velocities from HARPS-N and HIRES. We measure a planet mass of $6.91^{+0.75}_{-0.85}$ M$_{\oplus}$ which implies an iron core mass fraction of $20^{+15}_{-12}$% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like and we constrain a H/He envelope mass fraction to be $

Published
2020

156. Physical parameters of the multiplanet systems HD 106315 and GJ 9827

Author

Kosiarek, MR, Kosiarek, MR, Berardo, DA, Crossfield, IJM, Laguna, C, Piaulet, C, Akana Murphy, JM, Howell, SB, Henry, GW, Isaacson, H, Fulton, B, Weiss, LM, Petigura, EA, Behmard, A, Hirsch, LA, Teske, J, Burt, JA, Mills, SM, Chontos, A, Močnik, T, Howard, AW, Werner, M, Livingston, JH, Krick, J, Beichman, C, Gorjian, V, Kreidberg, L, Morley, C, Christiansen, JL, Morales, FY, Scott, NJ, Crane, JD, Wang, SX, Shectman, SA, Rosenthal, LJ, Grunblatt, SK, Rubenzahl, RA, Dalba, PA, Giacalone, S, Villanueva, CD, Liu, Q, Dai, F, Hill, ML, Rice, M, Kane, SR, Mayo, AW, Kosiarek, MR, Kosiarek, MR, Berardo, DA, Crossfield, IJM, Laguna, C, Piaulet, C, Akana Murphy, JM, Howell, SB, Henry, GW, Isaacson, H, Fulton, B, Weiss, LM, Petigura, EA, Behmard, A, Hirsch, LA, Teske, J, Burt, JA, Mills, SM, Chontos, A, Močnik, T, Howard, AW, Werner, M, Livingston, JH, Krick, J, Beichman, C, Gorjian, V, Kreidberg, L, Morley, C, Christiansen, JL, Morales, FY, Scott, NJ, Crane, JD, Wang, SX, Shectman, SA, Rosenthal, LJ, Grunblatt, SK, Rubenzahl, RA, Dalba, PA, Giacalone, S, Villanueva, CD, Liu, Q, Dai, F, Hill, ML, Rice, M, Kane, SR, and Mayo, AW

Abstract

HD 106315 and GJ 9827 are two bright, nearby stars that host multiple super-Earths and sub-Neptunes discovered by K2 that are well suited for atmospheric characterization. We refined the planets' ephemerides through Spitzer transits, enabling accurate transit prediction required for future atmospheric characterization through transmission spectroscopy. Through a multiyear high-cadence observing campaign with Keck/High Resolution Echelle Spectrometer and Magellan/Planet Finder Spectrograph, we improved the planets' mass measurements in anticipation of Hubble Space Telescope transmission spectroscopy. For GJ 9827, we modeled activity-induced radial velocity signals with a Gaussian process informed by the Calcium II H&K lines in order to more accurately model the effect of stellar noise on our data. We measured planet masses of Mb = 4.87 ± 0.37 M⊕, Mc = 1.92 ± 0.49 M⊕, and Md = 3.42 ± 0.62 M⊕. For HD 106315, we found that such activity radial velocity decorrelation was not effective due to the reduced presence of spots and speculate that this may extend to other hot stars as well (Teff > 6200 K). We measured planet masses of Mb = 10.5 ± 3.1 M⊕ and Mc = 12.0 ± 3.8 M⊕. We investigated all of the planets' compositions through comparison of their masses and radii to a range of interior models. GJ 9827 b and GJ 9827 c are both consistent with a 50/50 rock-iron composition, GJ 9827 d and HD 106315 b both require additional volatiles and are consistent with moderate amounts of water or hydrogen/helium, and HD 106315 c is consistent with a ∼10% hydrogen/helium envelope surrounding an Earth-like rock and iron core.

Published
2020

157. Status and future developments of integrated photonic spectrographs for astronomy and Earth and planetary sciences

Author

Soskind, Yakov, Busse, Lynda E., Jovanovic, N., Cvetojevic, N., Daal, M., Mazin, B., Moreira, R., Mawet, D., Vasisht, G., Beichman, C., Wallace, K., Jewell, J., Leifer, S., Dekany, R., Porter, M., Soskind, Yakov, Busse, Lynda E., Jovanovic, N., Cvetojevic, N., Daal, M., Mazin, B., Moreira, R., Mawet, D., Vasisht, G., Beichman, C., Wallace, K., Jewell, J., Leifer, S., Dekany, R., and Porter, M.

Abstract

The size and cost of astronomical instruments for extremely large telescopes (ELTs), are pushing the limits of what is feasible, requiring optical components at the very edge of achievable size and performance. Operating at the diffraction-limit, the realm of photonic technologies, allows for highly compact instruments to be realized. In particular, Integrated Photonic Spectrographs (IPSs) have the potential to replace an instrument the size of a car with one that can be held in the palm of a hand. This miniaturization in turn offers dramatic improvements in mechanical and thermal stability. Owing to the single-mode fiber feed, the performance of the spectrograph is decoupled from the telescope and the instruments point spread function can be calibrated with a much higher precision. These effects combined mean that an IPS can provide superior performance with respect to a classical bulk optic spectrograph. In this paper we provide a summary of efforts made to qualify IPSs for astronomical applications to date. These include the early characterization of arrayed waveguide gratings for multi-object injection and modifications to facilitate a continuous spectrum, to the integration of these devices into prototypical instruments and most recently the demonstration of a highly optimized instrument directly fed from an 8-m telescope. We will then outline development paths necessary for astronomy, currently underway, which include broadening operating bands, bandwidth, increasing resolution, implementing cross-dispersion on-chip and integrating these devices with other photonic technologies and detectors such as superconducting Microwave Kinetic Inductance Detector arrays. Although the focus of this work is on IPS applicability to astronomy, they may be even more ideally suited to Earth and planetary science applications.

Published
2020

158. The CARMENES search for exoplanets around M dwarfs

Author

Dreizler, S., primary, Crossfield, I. J. M., additional, Kossakowski, D., additional, Plavchan, P., additional, Jeffers, S. V., additional, Kemmer, J., additional, Luque, R., additional, Espinoza, N., additional, Pallé, E., additional, Stassun, K., additional, Matthews, E., additional, Cale, B., additional, Caballero, J. A., additional, Schlecker, M., additional, Lillo-Box, J., additional, Zechmeister, M., additional, Lalitha, S., additional, Reiners, A., additional, Soubkiou, A., additional, Bitsch, B., additional, Zapatero Osorio, M. R., additional, Chaturvedi, P., additional, Hatzes, A. P., additional, Ricker, G., additional, Vanderspek, R., additional, Latham, D. W., additional, Seager, S., additional, Winn, J., additional, Jenkins, J. M., additional, Aceituno, J., additional, Amado, P. J., additional, Barkaoui, K., additional, Barbieri, M., additional, Batalha, N. M., additional, Bauer, F. F., additional, Benneke, B., additional, Benkhaldoun, Z., additional, Beichman, C., additional, Berberian, J., additional, Burt, J., additional, Butler, R. P., additional, Caldwell, D. A., additional, Chintada, A., additional, Chontos, A., additional, Christiansen, J. L., additional, Ciardi, D. R., additional, Cifuentes, C., additional, Collins, K. A., additional, Collins, K. I., additional, Combs, D., additional, Cortés-Contreras, M., additional, Crane, J. D., additional, Daylan, T., additional, Dragomir, D., additional, Esparza-Borges, E., additional, Evans, P., additional, Feng, F., additional, Flowers, E. E., additional, Fukui, A., additional, Fulton, B., additional, Furlan, E., additional, Gaidos, E., additional, Geneser, C., additional, Giacalone, S., additional, Gillon, M., additional, Gonzales, E., additional, Gorjian, V., additional, Hellier, C., additional, Hidalgo, D., additional, Howard, A. W., additional, Howell, S., additional, Huber, D., additional, Isaacson, H., additional, Jehin, E., additional, Jensen, E. L. N., additional, Kaminski, A., additional, Kane, S. R., additional, Kawauchi, K., additional, Kielkopf, J. F., additional, Klahr, H., additional, Kosiarek, M. R., additional, Kreidberg, L., additional, Kürster, M., additional, Lafarga, M., additional, Livingston, J., additional, Louie, D., additional, Mann, A., additional, Madrigal-Aguado, A., additional, Matson, R. A., additional, Mocnik, T., additional, Morales, J. C., additional, Muirhead, P. S., additional, Murgas, F., additional, Nandakumar, S., additional, Narita, N., additional, Nowak, G., additional, Oshagh, M., additional, Parviainen, H., additional, Passegger, V. M., additional, Pollacco, D., additional, Pozuelos, F. J., additional, Quirrenbach, A., additional, Reefe, M., additional, Ribas, I., additional, Robertson, P., additional, Rodríguez-López, C., additional, Rose, M. E., additional, Roy, A., additional, Schweitzer, A., additional, Schlieder, J., additional, Shectman, S., additional, Tanner, A., additional, Şenavcı, H. V., additional, Teske, J., additional, Twicken, J. D., additional, Villasenor, J., additional, Wang, S. X., additional, Weiss, L. M., additional, Wittrock, J., additional, Yılmaz, M., additional, and Zohrabi, F., additional

Published
2020
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159. Estimate Low and High Order Wavefront Using P1640 Calibrator Measurements

Author

Zhai, C, Vasisht, G, Shao, M, Lockhart, T, Cady, E, Oppenheimer, B, Burruss, R, Roberts, J, Beichman, C, Brenner, D, Crepp, J, Dekany, R, Hillenbrand, L, Hinkley, S, Parry, I, Pueyo, L, Rice, E, Roberts, L. C. Jr, Sivaramakrishnan, A, Soummer, R, Tang, H, Vescelus, F, Wallace, K, and Zimmerman, N

Subjects
Astronomy
Abstract

P1640 high contrast imaging system on the Palomar 200 inch Telescope consists of an apodized-pupil Lyot coronagraph, the PALM-3000 adaptive optics (P3K-AO), and P1640 Calibrator (CAL). Science images are recorded by an integral field spectrograph covering J-H bands for detecting and characterizing stellar companions. With aberrations from atmosphere corrected by the P3K-AO, instrument performance is limited mainly by the quasi-static speckles due to noncommon path wavefront aberrations for the light to propagate to the P3K-AO wavefront sensor and to the coronagraph mask. The non-common path wavefront aberrations are sensed by CAL, which measures the post-coronagraph E-field using interferometry, and can be effectively corrected by offsetting the P3K-AO deformable mirror target position accordingly. Previously, we have demonstrated using CAL measurements to correct high order wavefront aberrations, which is directly connected to the static speckles in the image plane. Low order wavefront, on the other hand, usually of larger amplitudes, causes light to leak through the coronagraph making the whole image plane brighter. Knowledge error in low order wavefront aberrations can also affect the estimation of the high order wavefront. Even though, CAL is designed to sense efficiently high order wavefront aberrations, the low order wavefront front can be inferred with less sensitivity. Here, we describe our method for estimating both low and high order wavefront aberrations using CAL measurements by propagating the post-coronagraph E-field to a pupil before the coronagraph. We present the results from applying this method to both simulated and experiment data.

Published
2013

161. The HOSTS Survey for Exozodiacal Dust: Observational Results from the Complete Survey

Author

Ertel, S., primary, Defrère, D., additional, Hinz, P., additional, Mennesson, B., additional, Kennedy, G. M., additional, Danchi, W. C., additional, Gelino, C., additional, Hill, J. M., additional, Hoffmann, W. F., additional, Mazoyer, J., additional, Rieke, G., additional, Shannon, A., additional, Stapelfeldt, K., additional, Spalding, E., additional, Stone, J. M., additional, Vaz, A., additional, Weinberger, A. J., additional, Willems, P., additional, Absil, O., additional, Arbo, P., additional, Bailey, V. P., additional, Beichman, C., additional, Bryden, G., additional, Downey, E. C., additional, Durney, O., additional, Esposito, S., additional, Gaspar, A., additional, Grenz, P., additional, Haniff, C. A., additional, Leisenring, J. M., additional, Marion, L., additional, McMahon, T. J., additional, Millan-Gabet, R., additional, Montoya, M., additional, Morzinski, K. M., additional, Perera, S., additional, Pinna, E., additional, Pott, J.-U., additional, Power, J., additional, Puglisi, A., additional, Roberge, A., additional, Serabyn, E., additional, Skemer, A. J., additional, Su, K. Y. L., additional, Vaitheeswaran, V., additional, and Wyatt, M. C., additional

Published
2020
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163. A First Order Wavefront Estimation Algorithm for P1640 Calibrator

Author

Zhaia, C, Vasisht, G, Shao, M, Lockhart, T, Cady, E, Oppenheimer, B, Burruss, R, Roberts, J, Beichman, C, Brenner, D, Crepp, J, Dekany, R, Hinkley, S, Hillenbrand, L, Parry, I, Pueyo, L, Rice, E, Roberts, L. C. Jr, Sivaramakrishnan, A, Soummer, R, Vescelus, F, Wallace, K, and Zimmerman, N

Subjects
Astronomy
Abstract

P1640 calibrator is a wavefront sensor working with the P1640 coronagraph and the Palomar 3000 actuator adaptive optics system (P3K) at the Palomar 200 inch Hale telescope. It measures the wavefront by interfering post-coronagraph light with a reference beam formed by low-pass filtering the blocked light from the coronagraph focal plane mask. The P1640 instrument has a similar architecture to the Gemini Planet Imager (GPI) and its performance is currently limited by the quasi-static speckles due to non-common path wavefront errors, which comes from the non-common path for the light to arrive at the AO wavefront sensor and the coronagraph mask. By measuring the wavefront after the coronagraph mask, the non-common path wavefront error can be estimated and corrected by feeding back the error signal to the deformable mirror (DM) of the P3K AO system. Here, we present a first order wavefront estimation algorithm and an instrument calibration scheme used in experiments done recently at Palomar observatory. We calibrate the P1640 calibrator by measuring its responses to poking DM actuators with a sparse checkerboard pattern at different amplitudes. The calibration yields a complex normalization factor for wavefront estimation and establishes the registration of the DM actuators at the pupil camera of the P1640 calibrator, necessary for wavefront correction. Improvement of imaging quality after feeding back the wavefront correction to the AO system demonstrated the efficacy of the algorithm.

Published
2012

165. Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: A Sub-Jupiter Orbiting an M Dwarf in the Disk

Author

Calchi Novati, S., Beichman, C., Henderson, C. B., and Carey, S.

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the discovery of a sub-Jupiter-mass planet orbiting beyond the snow line of an M dwarf most likely in the Galactic disk as part of the joint Spitzer and ground-based monitoring of planetary microlensing anomalies toward the Galactic bulge. Most of the microlensing parameters are strongly constrained by the light-curve modeling, and in particular there is a Spitzer-based measurement of the microlens parallax, π E. However, there are no caustic crossings, so the angular Einstein radius has only an upper limit based on the light-curve modeling alone. Additionally, the analysis leads us to identify eight degenerate configurations: the fourfold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To calculate the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the χ 2 hierarchy, the Rich argument (stating that the small-parallax solution is more likely), and a prior Galactic model. The preferred configuration, favored by a likelihood ratio of at least 4000, is for a host at D_L = 3.73^(+0.66)_(-0.67) kpc with mass M_L = 0.30^(+0.15)_(-0.12) M⊙, orbited by a Saturn-like planet with M_(planet) = 0.43^(+0.21)_(-0.17) M_(Jup) at projected separation a = 1.70^(+0.38)_(-0.39) au, about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting beyond the snow line of M dwarfs discovered by microlensing. Based on the rules of the real-time protocol for the selection of events to be followed up with Spitzer, this planet will not enter the sample for measuring the Galactic distribution of planets.

Published
2019

166. OGLE-2018-BLG-0022: First Prediction of an Astrometric Microlensing Signal from a Photometric Microlensing Event

Author

Han, C., Bond, I., Udalski, A., Gould, A., Bozza, V., Hirao, Y., Cassan, A., authors, L., Albrow, M., Chung, S., Hwang, K., Lee, C., Ryu, Y., Shin, I., Shvartzvald, Y., Yee, J., Jung, Y., Kim, D., Kim, W., Cha, S., Kim, H., Kim, S., Lee, D., Lee, Y., Park, B., Pogge, R., Zang, W., Collaboration, T., Abe, F., Barry, R., Bennett, D., Bhattacharya, A., Donachie, M., Fukui, A., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N., Suematsu, H., Sullivan, D., Sumi, T., Suzuki, D., Tristram, P., Yonehara, A., Mróz, P., Szymański, M., Skowron, J., Poleski, R., Soszyński, I., Pietrukowicz, P., Kozłowski, S., Ulaczyk, K., Rybicki, K., Iwanek, P., Wrona, M., Beichman, C., Bryden, G., Carey, S., Gaudi, B., Henderson, C., and Team, S.

Abstract

In this work, we present the analysis of the binary microlensing event OGLE-2018-BLG-0022 that is detected toward the Galactic bulge field. The dense and continuous coverage with the high-quality photometry data from ground-based observations combined with the space-based Spitzer observations of this long timescale event enables us to uniquely determine the masses M 1 = 0.40 ± 0.05 M ☉ and M 2 = 0.13 ± 0.01 M ☉ of the individual lens components. Because the lens-source relative parallax and the vector lens-source relative proper motion are unambiguously determined, we can likewise unambiguously predict the astrometric offset between the light centroid of the magnified images (as observed by the Gaia satellite) and the true position of the source. This prediction can be tested when the individual-epoch Gaia astrometric measurements are released.

Published
2019

167. Spitzer Microlensing of MOA-2016-BLG-231L: A Counter-rotating Brown Dwarf Binary in the Galactic Disk

Author

Chung, S., Gould, A., Skowron, J., Bond, I., Zhu, W., Albrow, M., Jung, Y., Han, C., Hwang, K., Ryu, Y., Shin, I., Shvartzvald, Y., Yee, J., Zang, W., Cha, S., Kim, D., Kim, H., Kim, S., Kim, Y., Lee, C., Lee, D., Lee, Y., Park, B., Pogge, R., Collaboration, K., Udalski, A., Poleski, R., Mróz, P., Pietrukowicz, P., Szymański, M., Soszyński, I., Kozłowski, S., Ulaczyk, K., Pawlak, M., Collaboration, T., Beichman, C., Bryden, G., Calchi Novati, S., Carey, S., Gaudi, B., Henderson, C., Team, T., Abe, F., Barry, R., Bennett, D., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N., Suematsu, H., Sullivan, D., Sumi, T., Suzuki, D., Tristram, P., Yonehara, A., and MOA colllaboration, T.

Abstract

We analyze the binary microlensing event MOA-2016-BLG-231, which was observed from the ground and from Spitzer. The lens is composed of very- low-mass brown dwarfs (BDs) with {M}1={21}-5+12 {M}J and {M}2={9}-2+5 {M}J, and it is located in the Galactic disk {D}{{L}}={2.85}-0.50+0.88 {kpc}. This is the fifth binary brown dwarf discovered by microlensing, and the BD binary is moving counter to the orbital motion of disk stars. Constraints on the lens physical properties come from late-time, non- caustic-crossing features of the Spitzer light curve. Thus, MOA-2016-BLG-231 shows how Spitzer plays a crucial role in resolving the nature of BDs in binary BD events with short timescales (‚â≤10 days).

Published
2019

168. OGLE-2018-BLG-1011Lb,c: Microlensing Planetary System with Two Giant Planets Orbiting a Low-mass Star

Author

Han, C., Bennett, D., Udalski, A., Gould, A., Bond, I., Shvartzvald, Y., Nikolaus, K., Hundertmark, M., Bozza, V., Cassan, A., Hirao, Y., Bachelet, E., Fouqué, P., Authors, L., Albrow, M., Chung, S., Hong, K., Hwang, K., Lee, C., Ryu, Y., Shin, I., Yee, J., Jung, Y., Cha, S., Kim, D., Kim, H., Kim, S., Lee, D., Lee, Y., Park, B., Pogge, R., Collaboration, T., Mróz, P., Szymański, M., Skowron, J., Poleski, R., Soszyński, I., Pietrukowicz, P., Kozłowski, S., Ulaczyk, K., Rybicki, K., Iwanek, P., Wrona, M., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., Fukui, A., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N., Suematsu, H., Sullivan, D., Sumi, T., Suzuki, D., Tristram, P., Yonehara, A., Mao, S., Wang, T., Zang, W., Zhu, W., Penny, M., Beichman, C., Bryden, G., Calchi Novati, S., Gaudi, B., Henderson, C., Jacklin, S., Stassun, K., and Team, T.

Abstract

We report a multiplanetary system found from the analysis of microlensing event OGLE-2018-BLG-1011, for which the light curve exhibits a double-bump anomaly around the peak. We find that the anomaly cannot be fully explained by the binary-lens or binary-source interpretations and its description requires the introduction of an additional lens component. The 3L1S (three lens components and a single source) modeling yields three sets of solutions, in which one set of solutions indicates that the lens is a planetary system in a binary, while the other two sets imply that the lens is a multiplanetary system. By investigating the fits of the individual models to the detailed light curve structure, we find that the multiple-planet solution with planet- to-host mass ratios ∼9.5 10−3 and ∼15 10−3 are favored over the other solutions. From the Bayesian analysis, we find that the lens is composed of two planets with masses {1.8}-1.1+3..4 {M}{{J}} and {2.8}-1.7+5.1 {M}{{J}} around a host with a mass {0.18}-0.10+0.33 {M}ȯ and located at a distance {7.1}-1.5+1.1 {kpc}. The estimated distance indicates that the lens is the farthest system among the known multiplanetary systems. The projected planet-host separations are {a}\perp ,2={1.8}-1.5+2.1 {au} ({0.8}-0.6+0.9 {au}) and {a}\perp ,3={0.8}-0.6+0.9 {au}, where the values of a ⊥,2 inside and outside the parenthesis are the separations corresponding to the two degenerate solutions, indicating that both planets are located beyond the snow line of the host, as with the other four multiplanetary systems previously found by microlensing.

Published
2019

169. HD 2685 b: a hot Jupiter orbiting an early F-type star detected by TESS

Author

Ségransan, D., Pepe, F., Osip, D., Doty, J., Sedaghati, E., Relles, H., Ziegler, C., Tenenbaum, P., Jenkins, J.M., Nielsen, L.D., Cruz, B., Paredes, L.A., Sarkis, P., Matthews, E., Furész, G., Bayliss, D., Henning, T., Lovis, C., Haworth, K., Matson, R., Schlieder, J., Turner, O., Vanderburg, A., Law, N.M., Brahm, R., Jones, M.I., Bakos, G., Howell, S., Latham, D.W., Jordán, A., Dittmann, J., Christiansen, J.L., Mann, A.W., Gonzales, E., Henry, T., Hodari-Sadiki, J., Suc, V., Winn, J.N., Marmier, M., Tokovinin, A., Udry, S., Davies, M., Smith, J.C., Bouchy, F., Crossfield, I., Seager, S., Laughlin, G., Collins, K.A., Shporer, A., Wang, S., Espinoza, N., Beichman, C., and Ciardi, D.

Abstract

We report on the confirmation of a transiting giant planet around the relatively hot (Teff = 6801 ± 76 K) star HD 2685, whose transit signal was detected in Sector 1 data of NASA's TESS mission. We confirmed the planetary nature of the transit signal using Doppler velocimetric measurements with CHIRON, CORALIE, and FEROS, as well as using photometric data obtained with the Chilean-Hungarian Automated Telescope and the Las Cumbres Observatory. From the joint analysis of photometry and radial velocities, we derived the following parameters for HD 2685 b: P = 4.12688-0.00004+0.00005 days, e = 0.091-0.047+0.039, MP = 1.17 ± 0.12 MJ, and RP =1.44 ± 0.05 RJ. This system is a typical example of an inflated transiting hot Jupiter in a low- eccentricity orbit. Based on the apparent visual magnitude (V = 9.6 mag) of the host star, this is one of the brightest known stars hosting a transiting hot Jupiter, and it is a good example of the upcoming systems that will be detected by TESS during the two-year primary mission. This is also an excellent target for future ground- and space-based atmospheric characterization as well as a good candidate for measuring the projected spin-orbit misalignment angle through the Rossiter- McLaughlin effect. Tables of the photometry are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/625/A16

Published
2019

170. Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf

Author

Jung, Y., Gould, A., Udalski, A., Sumi, T., Yee, J., Shvartzvald, Y., Zang, W., Han, C., Albrow, M., Chung, S., Hwang, K., Ryu, Y., Shin, I., Zhu, W., Cha, S., Kim, D., Kim, H., Kim, S., Lee, C., Lee, D., Lee, Y., Park, B., Pogge, R., Mróz, P., Szymański, M., Skowron, J., Poleski, R., Soszyński, I., Pietrukowicz, P., Kozłowski, S., Ulaczyk, K., Rybicki, K., Iwanek, P., Wrona, M., Beichman, C., Bryden, G., Calchi Novati, S., Carey, S., Gaudi, B., Henderson, C., Abe, F., Barry, R., Bennett, D., Bond, I., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ranc, C., Rattenbury, N., Suematsu, H., Sullivan, D., Suzuki, D., Tristram, P., Yonehara, A., Jacklin, S., Penny, M., Stassun, K., Fouqué, P., Mao, S., and Wang, T.

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the discovery of a Spitzer microlensing planet OGLE-2018-BLG- 0596Lb, with preferred planet-host mass ratio q ∼ 2 10−4. The planetary signal, which is characterized by a short (∼1 day) “bump” on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a “Hollywood” geometry. Combined with the source proper motion measured from Gaia, the Spitzer satellite parallax measurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planet perturbs the minor image due to lensing by the host, yields a Uranus-mass planet with a mass of M p = 13.9 ± 1.6 M ⊕ orbiting a mid M-dwarf with a mass of M h = 0.23 ± 0.03 M ☉. There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planet perturbs the major image. The latter solution yields M p = 1.2 ± 0.2 M ⊕ and M h = 0.15 ± 0.02 M ☉. By combining the microlensing and Gaia data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance D L ∼ 6 ± 1 kpc. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy.

Published
2019

171. Terrestrial Planet Finder Interferometer: 2007-2008 Progress and Plans

Author

Lawson, P. R, Lay, O. P, Martin, S. R, Peters, R. D, Gappinger, R. O, Ksendzov, A, Scharf, D. P, Booth, A. J, Beichman, C. A, Serabyn, E, Johnston, K. J, and Danchi, W. C

Subjects
Lunar And Planetary Science And Exploration, Astronomy, Instrumentation And Photography
Abstract

This paper provides an overview of technology development for the Terrestrial Planet Finder Interferometer (TPF-I). TPF-I is a mid-infrared space interferometer being designed with the capability of detecting Earth-like planets in the habitable zones around nearby stars. The overall technology roadmap is presented and progress with each of the testbeds is summarized. The current interferometer architecture, design trades, and the viability of possible reduced-scope mission concepts are also presented.

Published
2008

173. Preliminary Results from the 2MASS Core Project

Author

Liebert, J., primary, Reid, I. N., additional, Kirkpatrick, J. D., additional, Cutri, R., additional, Nelson, B., additional, Beichman, C., additional, Monet, D. G., additional, Dahn, C. C., additional, Skrutskie, M., additional, Gizis, J. E., additional, and Fisher, M. D., additional

Published
2000
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175. OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Author

Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Yee, J. C., Novati, S. Calchi, Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bond, I. A., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Christie, G., Drummond, J., Green, J., Hennerley, S., Natusch, T., Porritt, I., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Bozza, V., Dominik, M., Hundertmark, M., Peixinho, N., Sajadian, S., Burgdorf, M. J., Evans, D. F., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Helling, C., Henning, T., Hinse, T. C., Mancini, L., Longa-Pena, P., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., Unda-Sanzana, E., von Essen, C., Beaulieu, J. -P., Blackman, J., Hill, K., Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Yee, J. C., Novati, S. Calchi, Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bond, I. A., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Christie, G., Drummond, J., Green, J., Hennerley, S., Natusch, T., Porritt, I., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Bozza, V., Dominik, M., Hundertmark, M., Peixinho, N., Sajadian, S., Burgdorf, M. J., Evans, D. F., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Helling, C., Henning, T., Hinse, T. C., Mancini, L., Longa-Pena, P., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., Unda-Sanzana, E., von Essen, C., Beaulieu, J. -P., Blackman, J., and Hill, K.

Published
2019

176. A Jovian planet in an eccentric 11.5 day orbit around HD 1397 discovered by TESS

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Nielsen, L. D., Bouchy, F., Turner, O., Giles, H., Mascareño, A. Suárez, Lovis, C., Marmier, M., Pepe, F., Ségransan, D., Udry, S., Otegi, J. F., Ottoni, G., Stalport, M., Ricker, George R, Vanderspek, Roland K, Latham, D. W., Seager, Sara, Winn, J. N., Jenkins, J. M., Kane, S. R., Wittenmyer, R. A., Bowler, B., Crossfield, Ian Jm, Horner, J., Kielkopf, J., Morton, T., Plavchan, P., Tinney, C. G., Zhang, Hui, Wright, D. J., Mengel, M. W., Clark, J. T., Okumura, J., Addison, B., Caldwell, D. A., Cartwright, S. M., Collins, K. A., Francis, James E, Guerrero, Natalia M., Huang, Chengxi, Matthews, Elisabeth C, Pepper, J., Rose, M., Villasenor, Jesus Noel Samonte, Wohler, B., Stassun, K., Howell, S., Ciardi, D., Gonzales, E., Matson, R., Beichman, C., Schlieder, J., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Nielsen, L. D., Bouchy, F., Turner, O., Giles, H., Mascareño, A. Suárez, Lovis, C., Marmier, M., Pepe, F., Ségransan, D., Udry, S., Otegi, J. F., Ottoni, G., Stalport, M., Ricker, George R, Vanderspek, Roland K, Latham, D. W., Seager, Sara, Winn, J. N., Jenkins, J. M., Kane, S. R., Wittenmyer, R. A., Bowler, B., Crossfield, Ian Jm, Horner, J., Kielkopf, J., Morton, T., Plavchan, P., Tinney, C. G., Zhang, Hui, Wright, D. J., Mengel, M. W., Clark, J. T., Okumura, J., Addison, B., Caldwell, D. A., Cartwright, S. M., Collins, K. A., Francis, James E, Guerrero, Natalia M., Huang, Chengxi, Matthews, Elisabeth C, Pepper, J., Rose, M., Villasenor, Jesus Noel Samonte, Wohler, B., Stassun, K., Howell, S., Ciardi, D., Gonzales, E., Matson, R., Beichman, C., and Schlieder, J.

Abstract

The Transiting Exoplanet Survey Satellite TESS has begun a new age of exoplanet discoveries around bright host stars. We present the discovery of HD 1397b (TOI-120.01), a giant planet in an 11.54-day eccentric orbit around a bright (V = 7.9) G-type subgiant. We estimate both host star and planetary parameters consistently using EXOFASTv2 based on TESS time-series photometry of transits and radial velocity measurements with CORALIE and MINERVA-Australis. We also present high angular resolution imaging with NaCo to rule out any nearby eclipsing binaries. We find that HD 1397b is a Jovian planet, with a mass of 0.415 ± 0.020 MJ and a radius of 1.026 ± 0.026 RJ. Characterising giant planets in short-period eccentric orbits, such as HD 1397b, is important for understanding and testing theories for the formation and migration of giant planets as well as planet-star interactions.

Published
2019

178. Planck 2015 results XXVI. The Second Planck Catalogue of Compact Sources

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Argüeso, F., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Beichman, C., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P, Bersanelli, M., Bielewicz, P., Bock, J. J., Böhringer, H., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F, Carvalho, P., Catalano, A., Challinor, A., Chamballu, A., Chary, R. -R, Chiang, H. C., Christensen, P. R., Clemens, M., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., Bernardis, P., Rosa, A., Zotti, G., Delabrouille, J., Désert, F. -X, Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M, Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., León-Tavares, J., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A, Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Negrello, M., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L, Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Sanghera, H. S., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A. -S, Sygnet, J. -F, Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tornikoski, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Tent, B., Vielva, P., Villa, F., Wade, L. A., Walter, B., Wandelt, B. D., Wehus, I. K., Yvon, D., Andrea Zacchei, Zonca, A., Ade, P. A. R., Aghanim, N., Arguëso, F., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Beichman, C., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bock, J. J., Böhringer, H., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. F., Carvalho, P., Catalano, A., Challinor, A., Chamballu, A., Chary, R. R., Chiang, H. C., Christensen, P. R., Clemens, M., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., León Tavares, J., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Negrello, M., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rowan Robinson, M., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Sanghera, H. S., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tornikoski, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Walter, B., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., Zonca, A., Ade, P, Aghanim, N, Arguëso, F, Arnaud, M, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Battaner, E, Beichman, C, Benabed, K, Benoît, A, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bock, J, Böhringer, H, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bucher, M, Burigana, C, Butler, R, Calabrese, E, Cardoso, J, Carvalho, P, Catalano, A, Challinor, A, Chamballu, A, Chary, R, Chiang, H, Christensen, P, Clemens, M, Clements, D, Colombi, S, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Désert, F, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, T, Eriksen, H, Falgarone, E, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Giard, M, Giraud Héraud, Y, Gjerløw, E, González Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Gruppuso, A, Gudmundsson, J, Hansen, F, Hanson, D, Harrison, D, Helou, G, Henrot Versillé, S, Hernández Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Hurier, G, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leahy, J, Leonardi, R, León Tavares, J, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, López Caniego, M, Lubin, P, Maciás Pérez, J, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Marshall, D, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Mcgehee, P, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville Deschênes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Negrello, M, Netterfield, C, Nørgaard Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Oxborrow, C, Paci, F, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, T, Perdereau, O, Perotto, L, Perrotta, F, Pettorino, V, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rowan Robinson, M, Rubinõ Martín, J, Rusholme, B, Sandri, M, Sanghera, H, Santos, D, Savelainen, M, Savini, G, Scott, D, Seiffert, M, Shellard, E, Spencer, L, Stolyarov, V, Sudiwala, R, Sunyaev, R, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tornikoski, M, Tristram, M, Tucci, M, Tuovinen, J, Türler, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, L, Walter, B, Wandelt, B, Wehus, I, Yvon, D, Zacchei, A, Zonca, A, Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Planck, Hélium : du fondamental aux applications (NEEL - HELFA), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Facilities Council (STFC), and Imperial College Trust

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, media_common.quotation_subject, radio continuum: general, FOS: Physical sciences, Flux, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, general [Submillimeter], Cosmology: observation, 01 natural sciences, Catalogs, Cosmology: observations, Radio continuum: general, Submillimeter: general, Astronomy and Astrophysics, Space and Planetary Science, catalogs, cosmology: observations, submillimeter: general, NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Planck, observations [Cosmology], GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, general [Radio continuum], 010308 nuclear & particles physics, Orientation (computer vision), Astrophysics::Instrumentation and Methods for Astrophysics, Planck temperature, Astronomy and Astrophysic, Polarization (waves), 0201 Astronomical And Space Sciences, Sky, astro-ph.CO, symbols, Catalog, Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

ASI, Agenzia Spaziale Italiana; CNR, Consiglio Nazionale delle Ricerche, Planck is a project of the European Space Agency in cooperation with the scientific community, which started in 1993. CSIC, MINECO, JA, and RES (Spain); ERC and PRACE (EU)., Ade, P.A.R., Aghanim, N., Arguëso, F., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Battaner, E., Beichman, C., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Böhringer, H., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Carvalho, P., Catalano, A., Challinor, A., Chamballu, A., Chary, R.-R., Chiang, H.C., Christensen, P.R., Clemens, M., Clements, D.L., Colombi, S., Colombo, L.P.L., Combet, C., Couchot, F., Coulais, A., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Désert, F.-X., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K.M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J.E., Hansen, F.K., Hanson, D., Harrison, D.L., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., León-Tavares, J., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vørnle, M., López-Caniego, M., Lubin, P.M., Maciás-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Marshall, D.J., Martin, P.G., Martínez-González, E., Masi, S., Matarrese, S., Mcgehee, P., Meinhold, P.R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J.A., Naselsky, P., Nati, F., Natoli, P., Negrello, M., Netterfield, C.B., Nørgaard-Nielsen, H.U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C.A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T.J., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Pratt, G.W., Prézeau, G., Prunet, S., Puget, J.-L., Rachen, J.P., Reach, W.T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rowan-Robinson, M., Rubinõ-Martín, J.A., Rusholme, B., Sandri, M., Sanghera, H.S., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M.D., Shellard, E.P.S., Spencer, L.D., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tornikoski, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Walter, B., Wandelt, B.D., Wehus, I.K., Yvon, D., Zacchei, A., Zonca, A.

Published
2016

184. Precursor Science for the Terrestrial Planet Finder

Author

Lawson, P. R, Unwin, S. C, and Beichman, C. A

Subjects
Astronomy
Abstract

This document outlines a path for the development of the field of extrasolar planet research, with a particular emphasis on the goals of the Terrestrial Planet Finder (TPF). Over the past decade, a new field of research has developed, the study of extrasolar planetary systems, driven by the discovery of massive planets around nearby stars. The planet count now stands at over 130. Are there Earth-like planets around nearby stars? Might any of those planets be conducive to the formation and maintenance of life? These arc the questions that TPF seeks to answer. TPF will be implemented as a suite of two space observatories, a 6-m class optical coronagraph, to be launched around 20 14, and a formation flying mid-infrared interferometer, to be launched sometime prior to 2020. These facilities will survey up to 165 or more nearby stars and detect planets like Earth should they be present in the 'habitable zone' around each star. With observations over a broad wavelength range, TPF will provide a robust determination of the atmospheric composition of planets to assess habitability and the presence of life. At this early stage of TPF's development, precursor observational and theoretical programs are essential to help define the mission, to aid our understanding of the planets that TPF could discover, and to characterize the stars that TPF will eventually study. This document is necessarily broad in scope because the significance of individual discoveries is greatly enhanced when viewed in thc context of the field as a whole. This document has the ambitious goal of taking us from our limited knowledge today, in 2004, to the era of TPF observations in the middle of the next decade. We must use the intervening years wisely. This document will be reviewed annually and updated as needed. The most recent edition is available online at http://tpf.jpl.nasa.gov/ or by email request to lawson@hucy.jpl.nasa.gov

Published
2004

185. Precursor science for the Terrestrial Planet Finder

Author

Beichman, C. A, Unwin, S. C, and Lawson, Peter R

Abstract

This document outlines a path for the development of the field of extrasolar planet research, with a particular emphasis on the goals of the Terrestrial Planet Finder (TPF). Over the past decade, a new field of research has developed, the study of extrasolar planetary systems, driven by the discovery of massive planets around nearby stars. The planet count now stands at over 130. Are there Earth-like planets around nearby stars? Might any of those planets be conducive to the formation and maintenance of life? These are the questions that TPF seeks to answer.

Published
2004

186. First look at the Fomalhaut debris disk with the Spitzer Space Telescope

Author

Young, E. T, Van Cleve, J, Noriega-Crespo, A, Muzerolle, J, Morrison, J. E, Misselt, K, Megeath, T, Latter, W. B, Keene, J, Gordon, K. D, Frayer, D. T, Engelbracht, C. W, Egami, E, Blaylock, M, Backus, C, Velusamy, T, Thomspson, T, Marengo, M, Cadien, J, Bendo, G, Stansberry, J. A, Padgett, D. L, Jura, M, Beichman, C. A, Werner, M. W, Hines, D. C, Su, K. Y. L, Rieke, G. H, Chen, C, Holmes, E. K, and Stapelfeldt, K. R

Abstract

We present Spitzer Space Telescope early release observations of Fomalhaut, a nearby A-type star with dusty circumstellar debris. The disk is spatially resolved at 24, 70, and 160 mu m using the Multiband Imaging Photometer for Spitzer (MIPS). While the disk orientation and outer radius are comparable to values measured in the submillimeter, the disk inner radius cannot be precisely defined: the central hole in the submillimeter ring is at least partially filled with emission from warm dust, seen in Spitzer Infrared Spectrograph (IRS)17.5-34 mu m spectra and MIPS 24 mu m images. The disk surface brightness becomes increasingly asymmetric toward shorter wavelengths, with the south-southeast ansa always brighter than the north-northwest one. This asymmetry may reflect perturbations on the disk by an unseen interior planet.

Published
2004

188. Recommended architectures for the Terrestrial Planet Finder

Author

Beichman, C

Subjects
Astronomy
Abstract

The primary conclusion from an intensive, two year period of study is that with suitable technology investment, starting now, a mission to detect terrestrial planets around nearby stars could be launched within a decade.

Published
2004

190. Terrestrial planet finder

Author

Lawson, P. R, Beichman, C. A, Coulter, D. R, and Lindensmith, C. A

Abstract

UNKNOWN

Published
2003

198. How many Earths are enough?

Author

Beichman, C. A

Abstract

In this paper, I discuss some of the parameters that bound the size of the TPF/Darwin sample and outline a science program to improve our knowledge so that we can make timely decisions about the scope and expense of TPF/Darwin.

Published
2003

200. Searching for life with the Terrestrial Planet Finder: Lagrange point options for a formation flying interferometer

Author

Beichman, C, Gomez, G, Lo, M, Masdemont, J, and Romans, L

Subjects
Lunar And Planetary Science And Exploration
Abstract

In this paper, we describe the mission design for TPF assuming a distributed spacecraft concept using formation flight around both a halo orbit around L2 as well as a heliocentric orbit. Although the mission architecture is still under study, the next two years will include study of four design cncepts and a downselect to two concepts around 2005.

Published
2002

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