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1. MINDS. JWST/MIRI Reveals a Dynamic Gas-rich Inner Disk inside the Cavity of SY Cha

Author

Kamber R. Schwarz, Thomas Henning, Valentin Christiaens, Danny Gasman, Matthias Samland, Giulia Perotti, Hyerin Jang, Sierra L. Grant, Benoît Tabone, Maria Morales-Calderón, Inga Kamp, Ewine F. van Dishoeck, Manuel Güdel, Pierre-Olivier Lagage, David Barrado, Alessio Caratti o Garatti, Adrian M. Glauser, Tom P. Ray, Bart Vandenbussche, L. B. F. M. Waters, Aditya M. Arabhavi, Jayatee Kanwar, Göran Olofsson, Donna Rodgers-Lee, Jürgen Schreiber, and Milou Temmink

Subjects
Protoplanetary disks, Infrared spectroscopy, James Webb Space Telescope, Molecular spectroscopy, Astrophysics, QB460-466
Abstract

SY Cha is a T Tauri star surrounded by a protoplanetary disk with a large cavity seen in the millimeter continuum but has the spectral energy distribution of a full disk. Here we report the first results from JWST/Mid-InfraRed Instrument (MIRI) Medium Resolution Spectrometer (MRS) observations taken as part of the MIRI mid-INfrared Disk Survey (MINDS) GTO Program. The much improved resolution and sensitivity of MIRI-MRS compared to Spitzer enables a robust analysis of the previously detected H _2 O, CO, HCN, and CO _2 emission as well as a marginal detection of C _2 H _2 . We also report the first robust detection of mid-infrared OH and rovibrational CO emission in this source. The derived molecular column densities reveal the inner disk of SY Cha to be rich in both oxygen- and carbon-bearing molecules. This is in contrast to PDS 70, another protoplanetary disk with a large cavity observed with JWST, which displays much weaker line emission. In the SY Cha disk, the continuum, and potentially the line, flux varies substantially between the new JWST observations and archival Spitzer observations, indicative of a highly dynamic inner disk.

Published
2024
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2. MINDS. JWST/MIRI Reveals a Dynamic Gas-rich Inner Disk inside the Cavity of SY Cha

Author

Schwarz, Kamber R., primary, Henning, Thomas, additional, Christiaens, Valentin, additional, Gasman, Danny, additional, Samland, Matthias, additional, Perotti, Giulia, additional, Jang, Hyerin, additional, Grant, Sierra L., additional, Tabone, Benoît, additional, Morales-Calderón, Maria, additional, Kamp, Inga, additional, van Dishoeck, Ewine F., additional, Güdel, Manuel, additional, Lagage, Pierre-Olivier, additional, Barrado, David, additional, o Garatti, Alessio Caratti, additional, Glauser, Adrian M., additional, Ray, Tom P., additional, Vandenbussche, Bart, additional, Waters, L. B. F. M., additional, Arabhavi, Aditya M., additional, Kanwar, Jayatee, additional, Olofsson, Göran, additional, Rodgers-Lee, Donna, additional, Schreiber, Jürgen, additional, and Temmink, Milou, additional

Published
2024
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3. PANCHROMATIC OBSERVATIONS AND MODELING OF THE HV TAU C EDGE-ON DISK

Author

Gaspard Duchêne, Maria Morales-Calderon, Timothy Y. Brooke, Christophe Pinte, Andrea M. Ghez, H. Maness, Hervé Bouy, D. Padgett, Alberto Noriega-Crespo, C. McCabe, Karl Stapelfeldt, François Ménard, Gilles Duvert, D. Barrado y Navascués, and Sebastian Wolf

Subjects
Physics, 010504 meteorology & atmospheric sciences, Opacity, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Protoplanetary disk, Position angle, 01 natural sciences, Radial velocity, Wavelength, Atmospheric radiative transfer codes, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

We present new high spatial resolution (, Comment: 26 pages, 11 figures, editorially accepted for publication in ApJ

Published
2010

4. Spitzer: Accretion in Low‐Mass Stars and Brown Dwarfs in the λ Orionis Cluster

Author

Amelia Bayo, Maria Morales-Calderon, Nuria Calvet, Lee Hartmann, G. Fazzio, D. Barrado y Navascues, T. Megeath, John Stauffer, and Lori Allen

Subjects
Physics, education.field_of_study, Astrophysics (astro-ph), Population, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, Accretion (astrophysics), Stars, Photometry (astronomy), Space and Planetary Science, education, Low Mass, Equivalent width
Abstract

We present multi-wavelength optical and infrared photometry of 170 previously known low mass stars and brown dwarfs of the 5 Myr Collinder 69 cluster (Lambda Orionis). The new photometry supports cluster membership for most of them, with less than 15% of the previous candidates identified as probable non-members. The near infrared photometry allows us to identify stars with IR excesses, and we find that the Class II population is very large, around 25% for stars (in the spectral range M0 - M6.5) and 40% for brown dwarfs, down to 0.04 Msun, despite the fact that the H(alpha) equivalent width is low for a significant fraction of them. In addition, there are a number of substellar objects, classified as Class III, that have optically thin disks. The Class II members are distributed in an inhomogeneous way, lying preferentially in a filament running toward the south-east. The IR excesses for the Collinder 69 members range from pure Class II (flat or nearly flat spectra longward of 1 micron), to transition disks with no near-IR excess but excesses beginning within the IRAC wavelength range, to two stars with excess only detected at 24 micron. Collinder 69 thus appears to be at an age where it provides a natural laboratory for the study of primordial disks and their dissipation., ApJ, in press

Published
2007

5. Spectroscopy of Very Low Mass Stars and Brown Dwarfs in IC 2391: Lithium Depletion and Hα Emission

Author

David Barrado y Navascués, Ray Jayawardhana, and John R. Stauffer

Subjects
Physics, Initial mass function, 010504 meteorology & atmospheric sciences, Astrophysics (astro-ph), Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Stellar classification, 01 natural sciences, Stars, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Low Mass, Pleiades, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Open cluster
Abstract

We have obtained intermediate-resolution optical spectroscopy of 44 candidate very low mass members of the nearby young open cluster IC2391. Of these, 26 spectra are totally new, 14 were already analyzed in a previous paper and another four are in common. These spectra, taken at the Cerro Tololo 4-meter and Magellan I and II telescopes, allow us to confirm 33 of them as likely cluster members, based on their spectral types, presence of Li, and Halpha emission. Among these new cluster members is CTIO-160 (M7), the first IC2391 candidate to satisfy all criteria for being a substellar member of the cluster, including detection of the Li 6708A doublet. With the enlarged membership, we are able to locate the lithium depletion boundary of the cluster more reliably than in the past. Based on comparison to several theoretical models, we derive an age of 50+-5 Myr for IC2391. We also estimate new ages for the Alpha Per and Pleiades clusters; our ages are 85+-10 Myr and 130+-20 Myr, respectively. We derive an estimate of the initial mass function of IC2391 that extends to below the substellar limit, and compare it to those of other well-studied young open clusters. The index of the power law mass function for IC2391 is alpha=0.96+-0.12, valid in the range 0.5 to 0.072 M(sun)., Astrophysical Journal, accepted June 18, 2004

Published
2004

6. AHubble Space TelescopeWide Field Planetary Camera 2 Survey for Brown Dwarf Binaries in the α Persei and Pleiades Open Clusters

Author

Eduardo L. Martín, S. E. Dahm, David Barrado y Navascues, Isabelle Baraffe, and Hervé Bouy

Subjects
Physics, Proper motion, 010504 meteorology & atmospheric sciences, Brown dwarf, Binary number, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Space and Planetary Science, Primary (astronomy), 0103 physical sciences, Cluster (physics), Spectroscopy, Pleiades, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Open cluster
Abstract

We present the results of a high-resolution imaging survey for brown dwarf (BD) binaries in two open clusters. The observations were carried out with WFPC2 onboard HST. Our sample consists of 8 BD candidates in the alpha Per cluster and 25 BD candidates in the Pleiades. We have resolved 4 binaries in the Pleiades with separations in the range 0".094--0".058, corresponding to projected separations between 11.7~AU and 7.2~AU. No binaries were found among the alpha Per targets. Three of the binaries have proper motions consistent with cluster membership in the Pleiades cluster, and for one of them we report the detection of Halpha in emission and LiI absorption obtained from Keck~II/ESI spectroscopy. One of the binaries does not have a proper motion consistent with Pleiades membership. We estimate that BD binaries wider than 12~AU are less frequent than 9% in the alphaPer and Pleiades clusters. This is consistent with an extension to substellar masses of a trend observed among stellar binaries: the maximum semimajor axis of binary systems decreases with decreasing primary mass. We find a binary frequency of 2 binaries over 13 BDs with confirmed proper motion membership in the Pleiades, corresponding to a binary fraction of 15%(1 sigma error bar +15%/-5%). These binaries are limited to the separation range 7-12~AU and their mass ratios are larger than 0.7. The relatively high binary frequency (>10%), the bias to separations smaller than about 15 AU and the trend to high mass ratios (q>0.7) are fundamental properties of BDs. Current theories of BD formation do not appear to provide a good description of all these properties.

Published
2003

8. From the Top to the Bottom of the Main Sequence: A Complete Mass Function of the Young Open Cluster M35

Author

Eduardo L. Martín, D. Barrado y Navascues, Jerome Bouvier, and John R. Stauffer

Subjects
Physics, Stellar population, Astrophysics (astro-ph), Diagram, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Square (algebra), Photometry (optics), Stars, Space and Planetary Science, Range (statistics), Cluster (physics), Open cluster
Abstract

We present very deep and accurate photometry of the open cluster M35 (VRIc filters). We have covered a region of 27.5x27.5 square arcmin. The data range from Ic=12.5 to 23.5 mag, and the color intervals are 0.4\le(V-I)c\le3.0, 0.5\le(R-I)c\le2.5. Roughly, these values span from 1.6 M_\odot down to the substellar limit. By using the location of the stars on color-magnitude and color-color diagrams, we have selected candidate members of this cluster. We have merged our sample with previously published data and obtained a color-magnitude diagram for the complete stellar population of the cluster, covering the spectral range early B - mid M. The Mass Function increases monotonically, when plotted in a log-log form, until it reaches ~0.8 M_\odot (\alpha=2.59). It remains shallower for less massive stars (\alpha=0.81 for 0.8-0.2 M_\odot), whereas a decrease ins observed for stars close to the substellar regime. The total mass of the cluster is ~1600 M_\odot in the area covered by this study., Comment: Accepted ApJ (Jan 10, 2001 issue)

Published
2001

9. Ages of A‐Type Vega‐like Stars fromuvbyβ Photometry

Author

Inseok Song, David Barrado y Navascues, John Stauffer, and Jean-Pierre Caillault

Subjects
Photometry (optics), Physics, Stars, Age differences, Space and Planetary Science, Vega, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We have estimated the ages of a sample of A-type Vega-like stars by using Stromgren \emph{uvby$\beta} photometric data and theoretical evolutionary tracks. We find that 13 percent of these A stars have been reported as Vega-like stars in the literature and that the ages of this subset run the gamut from very young (50~Myr) to old (1~Gyr), with no obvious age difference compared to those of field A stars. We clearly show that the fractional IR luminosity decreases with the ages of Vega-like stars.

Published
2001

10. Ages of Late Spectral Type Vega-like Stars

Author

John R. Stauffer, Inseok Song, Sofia Randich, David Barrado y Navascués, and Jean-Pierre Caillault

Subjects
Physics, education.field_of_study, Astrophysics (astro-ph), Population, Vega, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Star system, Luminosity, Stars, Space and Planetary Science, Magnitude (astronomy), Angstrom, education
Abstract

We have estimated the ages of eight late-type Vega-like stars by using standard age dating methods for single late-type stars, e.g., location on the color magnitude diagram, Li 6708 angstrom absorption, CaII H&K emission, X-ray luminosity, and stellar kinematic population. With the exception of the very unusual pre-main sequence star system HD 98800, all the late-type Vega-like stars are the same age as the Hyades cluster (600-800 Myr) or older., 6 pages text, 5 figures, to be appeared in the ApJ Letters

Published
2000

11. The Age of β Pictoris

Author

Inseok Song, David Barrado y Navascués, John R. Stauffer, and Jean-Pierre Caillault

Subjects
Physics, Photometry (optics), Young age, Stars, Space and Planetary Science, Error bar, Order (group theory), Beta Pictoris, Astronomy and Astrophysics, Beta Pictoris moving group, Astrophysics, Effective temperature
Abstract

We have reanalyzed data for the proposed moving group associated with β Pictoris in order to determine if the group (or part of it) is real and, if so, to derive an improved age estimate for β Pic. By using new, more accurate proper motions from PPM and Hipparcos and a few new radial velocities, we conclude that on kinematic grounds, most of the proposed members of the moving group are not, in fact, associated with β Pic. However, two M dwarfs—or three, actually, since one of them is a nearly equal mass binary—have space motions that coincide with that of β Pic to within 1 km s-1 with small error bars. Based on a color-magnitude diagram derived from accurate photometry and Hipparcos parallaxes, these two possible proper-motion companions to β Pic are very young; we derive an age of ~20 Myr by comparison with theoretical tracks from F. D'Antona & I. Mazzitelli. In fact, the proposed β Pic companions comprise two of the three youngest M dwarfs in the sample of 160 dM stars for which we have data. The chromospheric and coronal activities of these two stars also confirm that they are quite young. We argue that the probability that two of the three youngest nearby M dwarfs would accurately share the space motion of β Pic by chance is quite small, and therefore we believe that β Pic and the two M dwarfs (GL 799 and GL 803) were formed together. The estimated age for β Pic is then 20 ± 10 Myr, where the uncertainty in the age arises primarily from possible errors in the pre-main-sequence isochrones and in the conversion from color to effective temperature. This young age for β Pic supports the contention that the IR excess for the Vega-like stars is age dependent.

Published
1999

12. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

Author

Santerne, A., primary, Hébrard, G., additional, Lillo-Box, J., additional, Armstrong, D. J., additional, Barros, S. C. C., additional, Demangeon, O., additional, Barrado, D., additional, Debackere, A., additional, Deleuil, M., additional, Mena, E. Delgado, additional, Montalto, M., additional, Pollacco, D., additional, Osborn, H. P., additional, Sousa, S. G., additional, Abe, L., additional, Adibekyan, V., additional, Almenara, J.-M., additional, André, P., additional, Arlic, G., additional, Barthe, G., additional, Bendjoya, P., additional, Behrend, R., additional, Boisse, I., additional, Bouchy, F., additional, Boussier, H., additional, Bretton, M., additional, Brown, D. J. A., additional, Carry, B., additional, Cailleau, A., additional, Conseil, E., additional, Coulon, G., additional, Courcol, B., additional, Dauchet, B., additional, Dalouzy, J.-C., additional, Deldem, M., additional, Desormières, O., additional, Dubreuil, P., additional, Fehrenbach, J.-M., additional, Ferratfiat, S., additional, Girelli, R., additional, Gregorio, J., additional, Jaecques, S., additional, Kugel, F., additional, Kirk, J., additional, Labrevoir, O., additional, Lachurié, J.-C., additional, Lam, K. W. F., additional, Guen, P. Le, additional, Martinez, P., additional, Maurin, L. P. A., additional, McCormac, J., additional, Pioppa, J-B., additional, Quadri, U., additional, Rajpurohit, A., additional, Rey, J., additional, Rivet, J.-P., additional, Roy, R., additional, Santos, N. C., additional, Signoret, F., additional, Strabla, L., additional, Suarez, O., additional, Toublanc, D., additional, Tsantaki, M., additional, Vienney, J.-M., additional, Wilson, P. A., additional, Bachschmidt, M., additional, Colas, F., additional, Gerteis, O., additional, Louis, P., additional, Mario, J.-C., additional, Marlot, C., additional, Montier, J., additional, Perroud, V., additional, Pic, V., additional, Romeuf, D., additional, Ubaud, S., additional, and Verilhac, D., additional

Published
2016
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13. HII 2407: AN ECLIPSING BINARY REVEALED BY K2 OBSERVATIONS OF THE PLEIADES

Author

David, Trevor J., primary, Stauffer, John, additional, Hillenbrand, Lynne A., additional, Cody, Ann Marie, additional, Conroy, Kyle, additional, Stassun, Keivan G., additional, Pope, Benjamin, additional, Aigrain, Suzanne, additional, Gillen, Ed, additional, Cameron, Andrew Collier, additional, Barrado, David, additional, Rebull, L. M., additional, Isaacson, Howard, additional, Marcy, Geoffrey W., additional, Zhang, Celia, additional, Riddle, Reed L., additional, Ziegler, Carl, additional, Law, Nicholas M., additional, and Baranec, Christoph, additional

Published
2015
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14. Results of a Deep Imaging Survey of One Square Degree of the Pleiades for Low‐Luminosity Cluster Members

Author

John R. Stauffer, Leonardo Vanzi, J. Davy Kirkpatrick, Anna M. Angelova, Dana E. Backman, Rudolph E. Schild, David Barrado y Navascues, and Nigel Hambly

Subjects
Physics, Photometry (optics), Space and Planetary Science, Brown dwarf, Astronomy, Astronomy and Astrophysics, Astrophysics, Pleiades, Low Mass, Equivalent width, Spectrograph, Open cluster, Square degree
Abstract

We have obtained relatively deep imaging in two colors, with limiting magnitudes of V ~ 22.5 and Ic ~ 21, of about one square degree of the Pleiades open cluster. Our primary goal was to identify new candidate brown dwarf members of this ~100 Myr-old open cluster. In the process, we have also obtained V and Ic photometry for a large number of brighter proper-motion members of the cluster for which only photographic photometry had been available up until now. We identify six candidate objects whose locations in a V versus (V - I)c color-magnitude diagram are consistent with their being Pleiades members near or below the hydrogen-burning mass limit. We have obtained near-infrared photometry for several of these brown dwarf candidates, as well as for a selection of previously identified very low mass Pleiades members, and we use this new photometry to help determine whether the objects identified in the visual are indeed Pleiades members or not. Finally, we have obtained a moderate-resolution spectrum of one of the new brown dwarf candidates with the Keck LRIS spectrograph. The spectrum shows that the star has a spectral type of M7, which is compatible with its photometric colors, and that it has an Hα equivalent width of about 14 A and a marginally detected lithium 6708 A absorption equivalent width of about 0.4 A. These spectroscopic characteristics suggest that this object (MHObd1) is indeed a Pleiades member with a mass at or slightly above the hydrogen-burning mass limit.

Published
1998

15. The Age of Gliese 879 and Fomalhaut

Author

John R. Stauffer, D. Barrado y Navascues, Lee Hartmann, and Suchitra C. Balachandran

Subjects
Physics, Proper motion, Hertzsprung–Russell diagram, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, symbols.namesake, Stars, Fomalhaut, Space and Planetary Science, symbols, Astrophysics::Solar and Stellar Astrophysics, Circumstellar dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We estimate here the age of one of the prototypes of the Beta Pic-like stars, Fomalhaut, based on the properties of its common proper motion companion Gl879. By combining constraints derived from the lithium abundance, rotational velocity, HR diagram position, and coronal activity we conclude that the age for Gl879, and hence the age for Fomalhaut, is 200$\pm$100 Myr. This age estimate agrees quite well with the completely independent age estimate derived directly from isochrone--fitting to Fomalhaut's position in an HR diagram, and thus confirms that circumstellar dust disks can persist in A stars for several hundred Myr.

Published
1997

16. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

Author

A. Santerne, G. Hébrard, J. Lillo-Box, D. J. Armstrong, S. C. C. Barros, O. Demangeon, D. Barrado, A. Debackere, M. Deleuil, E. Delgado Mena, M. Montalto, D. Pollacco, H. P. Osborn, S. G. Sousa, L. Abe, V. Adibekyan, J.-M. Almenara, P. André, G. Arlic, G. Barthe, P. Bendjoya, R. Behrend, I. Boisse, F. Bouchy, H. Boussier, M. Bretton, D. J. A. Brown, B. Carry, A. Cailleau, E. Conseil, G. Coulon, B. Courcol, B. Dauchet, J.-C. Dalouzy, M. Deldem, O. Desormières, P. Dubreuil, J.-M. Fehrenbach, S. Ferratfiat, R. Girelli, J. Gregorio, S. Jaecques, F. Kugel, J. Kirk, O. Labrevoir, J.-C. Lachurié, K. W. F. Lam, P. Le Guen, P. Martinez, L. P. A. Maurin, J. McCormac, J-B. Pioppa, U. Quadri, A. Rajpurohit, J. Rey, J.-P. Rivet, R. Roy, N. C. Santos, F. Signoret, L. Strabla, O. Suarez, D. Toublanc, M. Tsantaki, J.-M. Vienney, P. A. Wilson, M. Bachschmidt, F. Colas, O. Gerteis, P. Louis, J.-C. Mario, C. Marlot, J. Montier, V. Perroud, V. Pic, D. Romeuf, S. Ubaud, D. Verilhac, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Virologia, Laboratorio Nacional de Investigacao Veterinaria (LNIV), 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), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Geneva Observatory, University of Geneva [Switzerland], CdR & CdL group, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire Chante-Perdrix, School of Physics and Astronomy [Cardiff], Cardiff University, Hôpital Européen Georges Pompidou [APHP] (HEGP), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département RadioChimie et Procédés (DRCP), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval [Québec] (ULaval), Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), Universidade do Porto [Porto], Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval, Departamento de Física e Astronomia [Porto], Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), LAEX, Depto. Astrofísica, Centro de Astrobiología, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofisica de Canarias ( IAC ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Université Côte d'Azur ( UCA ), Observatoire de Haute-Provence ( OHP ), Institut Pythéas ( OSU PYTHEAS ), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), School of Physis & Astronomy, Hôpital Européen Georges Pompidou [APHP] ( HEGP ), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux ( EPOC ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -École pratique des hautes études ( EPHE ) -Centre National de la Recherche Scientifique ( CNRS ), Département RadioChimie et Procédés ( DRCP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables ( CdR & CdL group ), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Genève = University of Geneva (UNIGE), Environnements et Paléoenvironnements OCéaniques (EPOC), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École Pratique des Hautes Études (EPHE), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto-Universidade do Porto, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
Physics, 010308 nuclear & particles physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Stellar rotation, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, 01 natural sciences, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Magnitude (astronomy), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Visual binary
Abstract

International audience; In the present paper we report the discovery of a new hot Jupiter, K2-29 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25 days, a mass of 0.73 +/- 0.04M(sic), and a radius of 1.19 +/- 0.02 R(sic). The host star is a relatively bright (V = 12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of lithium, we find that the system might be as young as similar to 450 Myr. The observation of the Rossiter-McLaughlin effect shows that the planet is aligned with respect to the stellar spin. Given the deep transit (20 mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where both stars are relatively bright.

Published
2016

17. FIRST DETECTION OF THERMAL RADIOJETS IN A SAMPLE OF PROTO-BROWN DWARF CANDIDATES

Author

Morata, Oscar, primary, Palau, Aina, additional, González, Ricardo F., additional, Gregorio-Monsalvo, Itziar de, additional, Ribas, Álvaro, additional, Perger, Manuel, additional, Bouy, Hervé, additional, Barrado, David, additional, Eiroa, Carlos, additional, Bayo, Amelia, additional, Huélamo, Nuria, additional, Morales-Calderón, María, additional, and Rodríguez, Luís F., additional

Published
2015
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18. FIRST DETECTION OF THERMAL RADIOJETS IN A SAMPLE OF PROTO-BROWN DWARF CANDIDATES

Author

David Barrado, Oscar Morata, Manuel Perger, Álvaro Ribas, Luis F. Rodríguez, Carlos Eiroa, Aina Palau, Hervé Bouy, Itziar de Gregorio-Monsalvo, Nuria Huélamo, Amelia Bayo, Maria Morales-Calderon, Ricardo F. González, and UAM. Departamento de Física Teórica

Subjects
Stars: formation, Astrophysics::High Energy Astrophysical Phenomena, Young stellar object, Brown dwarf, individual objects (J041757, J041836, J041847, J041938) [ISM], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stars: protostars, Luminosity, Jansky, protostars [Stars], Astrophysics::Solar and Stellar Astrophysics, Protostar, Radio continuum: ISM, formation [Stars], Astrophysics::Galaxy Astrophysics, Physics, jets and outflows [ISM], Física, Astronomy and Astrophysics, ISM [Radio continuum], Stars, ISM: jets and outflows, Space and Planetary Science, Spectral energy distribution, Outflow, ISM: individual objects (J041757, J041836, J041847, J041938), Astrophysics::Earth and Planetary Astrophysics
Abstract

The Astrophysical Journal 807.1 (2015): 55 reproduced by permission of the AAS, We observed with the Jansky Very Large Array at 3.6 and 1.3 cm a sample of 11 proto-brown dwarf (BD) candidates in Taurus in a search for thermal radio jets driven by the most embedded BDs. We detected for the first time four thermal radio jets in proto-BD candidates. We compiled data from UKIDSS, 2MASS, Spitzer, WISE, and Herschel to build the spectral energy distribution (SED) of the objects in our sample, which are similar to typical Class I SEDs of young stellar objects (YSOs). The four proto-BD candidates driving thermal radio jets also roughly follow the well-known trend of centimeter luminosity against bolometric luminosity determined for YSOs, assuming they belong to Taurus, although they present some excess of radio emission compared to the known relation for YSOs. Nonetheless, we are able to reproduce the flux densities of the radio jets modeling the centimeter emission of the thermal radio jets using the same type of models applied to YSOs, but with corresponding smaller stellar wind velocities and mass-loss rates, and exploring different possible geometries of the wind or outflow from the star. Moreover, we also find that the modeled mass outflow rates for the bolometric luminosities of our objects agree reasonably well with the trends found between the mass outflow rates and bolometric luminosities of YSOs, which indicates that, despite the "excess" centimeter emission, the intrinsic properties of proto-BDs are consistent with a continuation of those of very low-mass stars to a lower mass range. Overall, our study favors the formation of BDs as a scaled-down version of low-mass stars, This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. O. Morata is supported by the MOST (Ministry of Science and Technology, Taiwan) ALMA-T grant MOST 103-2119-M-001-010-MY to the Institute of Astronomy & Astrophysics, Academia Sinica. A. Palau acknowledges financial support from UNAM-DGAPA-PAPIIT IA102815 grant, México. I. de Gregorio is supported by MICINN (Spain) grant AYA2011-30228-C03-01. R.F. González is funded by UNAM/PAPIIT grant IN112014. H. Bouy is funded by the the Ramón y Cajal fellowship program number RYC-2009-04497. H. Bouy, D. Barrado, N. Huélamo, and M. Morales Calderón are supported by MICINN (Spain) grant AYA2012-38897-C02-01. A. Bayo acknowledges financial support from the Proyecto Fondecyt de Iniciación 11140572. L. F. Rodríguez acknowledges the financial support from UNAM, and CONACyT, México

Published
2015

19. HERSCHEL/PACS SURVEY OF PROTOPLANETARY DISKS IN TAURUS/AURIGA—OBSERVATIONS OF [O I] AND [C II], AND FAR-INFRARED CONTINUUM

Author

Howard, Christian D., primary, Sandell, Göran, additional, Vacca, William D., additional, Duchêne, Gaspard, additional, Mathews, Geoffrey, additional, Augereau, Jean-Charles, additional, Barrado, David, additional, Dent, William R. F., additional, Eiroa, Carlos, additional, Grady, Carol, additional, Kamp, Inga, additional, Meeus, Gwendolyn, additional, Ménard, Francois, additional, Pinte, Christophe, additional, Podio, Linda, additional, Riviere-Marichalar, Pablo, additional, Roberge, Aki, additional, Thi, Wing-Fai, additional, Vicente, Silvia, additional, and Williams, Jonathan P., additional

Published
2013
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21. YSOVAR: THE FIRST SENSITIVE, WIDE-AREA, MID-INFRARED PHOTOMETRIC MONITORING OF THE ORION NEBULA CLUSTER

Author

Morales-Calderón, M., primary, Stauffer, J. R., additional, Hillenbrand, L. A., additional, Gutermuth, R., additional, Song, I., additional, Rebull, L. M., additional, Plavchan, P., additional, Carpenter, J. M., additional, Whitney, B. A., additional, Covey, K., additional, de Oliveira, C. Alves, additional, Winston, E., additional, McCaughrean, M. J., additional, Bouvier, J., additional, Guieu, S., additional, Vrba, F. J., additional, Holtzman, J., additional, Marchis, F., additional, Hora, J. L., additional, Wasserman, L. H., additional, Terebey, S., additional, Megeath, T., additional, Guinan, E., additional, Forbrich, J., additional, Huélamo, N., additional, Riviere-Marichalar, P., additional, Barrado, D., additional, Stapelfeldt, K., additional, Hernández, J., additional, Allen, L. E., additional, Ardila, D. R., additional, Bayo, A., additional, Favata, F., additional, James, D., additional, Werner, M., additional, and Wood, K., additional

Published
2011
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22. DEBRIS DISKS OF MEMBERS OF THE BLANCO 1 OPEN CLUSTER,

Author

Stauffer, John R., primary, Rebull, Luisa M., additional, James, David, additional, Noriega-Crespo, Alberto, additional, Strom, Steven, additional, Wolk, Scott, additional, Carpenter, John M., additional, Barrado y Navascues, David, additional, Micela, Giusi, additional, Backman, Dana, additional, and Cargile, P. A., additional

Published
2010
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23. PANCHROMATIC OBSERVATIONS AND MODELING OF THE HV TAU C EDGE-ON DISK

Author

Duchêne, G., primary, McCabe, C., additional, Pinte, C., additional, Stapelfeldt, K. R., additional, Ménard, F., additional, Duvert, G., additional, Ghez, A. M., additional, Maness, H. L., additional, Bouy, H., additional, Barrado y Navascués, D., additional, Morales-Calderón, M., additional, Wolf, S., additional, Padgett, D. L., additional, Brooke, T. Y., additional, and Noriega-Crespo, A., additional

Published
2010
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24. MID-INFRARED VARIABILITY OF PROTOSTARS IN IC 1396A

Author

Morales-Calderón, M., primary, Stauffer, J. R., additional, Rebull, L., additional, Whitney, B. A., additional, Barrado y Navascués, D., additional, Ardila, D. R., additional, Song, I., additional, Brooke, T. Y., additional, Hartmann, L., additional, and Calvet, N., additional

Published
2009
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25. FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITHSWIFTX-RAY TRANSIENT 080109

Author

Modjaz, M., primary, Li, W., additional, Butler, N., additional, Chornock, R., additional, Perley, D., additional, Blondin, S., additional, Bloom, J. S., additional, Filippenko, A. V., additional, Kirshner, R. P., additional, Kocevski, D., additional, Poznanski, D., additional, Hicken, M., additional, Foley, R. J., additional, Stringfellow, G. S., additional, Berlind, P., additional, Barrado y Navascues, D., additional, Blake, C. H., additional, Bouy, H., additional, Brown, W. R., additional, Challis, P., additional, Chen, H., additional, de Vries, W. H., additional, Dufour, P., additional, Falco, E., additional, Friedman, A., additional, Ganeshalingam, M., additional, Garnavich, P., additional, Holden, B., additional, Illingworth, G., additional, Lee, N., additional, Liebert, J., additional, Marion, G. H., additional, Olivier, S. S., additional, Prochaska, J. X., additional, Silverman, J. M., additional, Smith, N., additional, Starr, D., additional, Steele, T. N., additional, Stockton, A., additional, Williams, G. G., additional, and Wood-Vasey, W. M., additional

Published
2009
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26. New Young Brown Dwarfs in the Orion Molecular Cloud 2/3 Region

Author

Peterson, Dawn E., primary, Megeath, S. T., additional, Luhman, K. L., additional, Pipher, J. L., additional, Stauffer, J. R., additional, Barrado y Navascués, D., additional, Wilson, J. C., additional, Skrutskie, M. F., additional, Nelson, M. J., additional, and Smith, J. D., additional

Published
2008
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28. A Sensitive Search for Variability in Late L Dwarfs: The Quest for Weather

Author

Morales-Calderón, M., primary, Stauffer, J. R., additional, Kirkpatrick, J. Davy, additional, Carey, S., additional, Gelino, C. R., additional, Navascués, D. Barrado y, additional, Rebull, L., additional, Lowrance, P., additional, Marley, M. S., additional, Charbonneau, D., additional, Patten, B. M., additional, Megeath, S. T., additional, and Buzasi, D., additional

Published
2006
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35. A Sensitive Search for Variability in Late L Dwarfs: The Quest for Weather

Author

David Charbonneau, Patrick Lowrance, Derek Buzasi, Luisa Rebull, D. Barrado y Navascués, Sean Carey, John R. Stauffer, Mark S. Marley, S. T. Megeath, Brian M. Patten, Maria Morales-Calderon, J. Davy Kirkpatrick, and Christopher R. Gelino

Subjects
Rotation period, Physics, Astrophysics (astro-ph), Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, Monitoring program, Root mean square, Photometry (optics), Wavelength, Amplitude, Space and Planetary Science
Abstract

We have conducted a photometric monitoring program of 3 field late-L brown dwarfs looking for evidence of non-axisymmetric structure or temporal variability in their photospheres. The observations were performed using Spitzer/IRAC 4.5 and 8 micron bandpasses and were designed to cover at least one rotational period of each object. One-sigma RMS (root mean squared) uncertainties of less than 3 mmag at 4.5 micron and around 9 mmag at 8 micron were achieved. Two out of the three objects studied exhibit some modulation in their light curves at 4.5 micron - but not 8 micron - with periods of 7.4 hr and 4.6 hr and peak-to-peak amplitudes of 10 mmag and 8 mmag. Although the lack of detectable 8 micron variation suggests an instrumental origin for the detected variations, the data may nevertheless still be consistent with intrinsic variability since the shorter wavelength IRAC bandpasses probe more deeply into late L dwarf atmospheres than the longer wavelengths. A cloud feature occupying a small percentage (1-2 %) of the visible hemisphere could account for the observed amplitude of variation. If, instead, the variability is indeed instrumental in origin, then our non-variable L dwarfs could be either completely covered with clouds or objects whose clouds are smaller and uniformly distributed. Such scenarios would lead to very small photometric variations. Followup IRAC photometry at 3.6 and 5.8 micron bandpasses should distinguish between the two cases. In any event, the present observations provide the most sensitive search to date for structure in the photospheres of late-L dwarfs at mid-IR wavelengths, and our photometry provides stringent upper limits to the extent to which the photospheres of these transition L dwarfs are structured., Comment: Accepted by ApJ. 16 pages, 6 figures

Published
2006

42. The Substellar Mass Function in σ Orionis

Author

Bejar, V. J. S., primary, Martin, E. L., additional, Osorio, M. R. Zapatero, additional, Rebolo, R., additional, Navascues, D. Barrado y, additional, Bailer‐Jones, C. A. L., additional, Mundt, R., additional, Baraffe, I., additional, Chabrier, C., additional, and Allard, F., additional

Published
2001
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49. Keck Spectra of Brown Dwarf Candidates and a Precise Determination of the Lithium Depletion Boundary in the α Persei Open Cluster

Author

Stauffer, John R., primary, Navascues, David Barrado y, additional, Bouvier, Jerome, additional, Morrison, Heather L., additional, Harding, Paul, additional, Luhman, K. L., additional, Stanke, Thomas, additional, McCaughrean, Mark, additional, Terndrup, Donald M., additional, Allen, Lori, additional, and Assouad, Patrick, additional

Published
1999
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