An Infrared Coronagraphic Survey for Substellar Companions

Lowrance, P.; Becklin, E. E.; Schneider, Glenn; Kirkpatrick, J. Davy; Weinberger, Alycia J.; Zuckerman, B.; Dumas, Christophe; Beuzit, Jean-Luc; Plait, P.; Malumuth, E. M.; Heap, S. R.; Terrile, R. J.; Hines, Dean C.

doi:10.1086/432839

Cited by 106 publications

(126 citation statements)

References 79 publications

Supporting

Mentioning

118

Contrasting

Order By: Relevance

“…5 of motion observed). Therefore, our astrometry proves that the NICMOS companions of Lowrance et al (2005) appear to be faint background objects unrelated to HR 8799A (see Table 1 for a detailed list of our astrometric measurements). October 25 data set (this FOV is roughly traced by the "B" green circle in Figure 3).…”

Section: Are "Hr 8799b" and "Hr 8799c" Background?supporting

confidence: 65%

“…On 1998 October 30 UT, HST/NICMOS observed HR 8799 with its coronagraph, and two candidate companions were identified (Lowrance et al 2005) in the roll-subtracted images. These faint point sources where reported at 13.…”

Section: Observations and Reductionsmentioning

confidence: 99%

“…Then in normal ADI one must subtract the master PSF from each individual frame after a cross-correlation alignment of each frame as in Close et al (2002). However, in WiFi ADI, the master PSF is created from non-aligned frames, then this PSF is subtracted off the individual images, in this manner all the bad pixels are optimally subtracted (since there are no image (Lowrance et al 2005) and Gemini Deep Planet Survey (Lafreniere et al 2007a), combined, binned by galactic latitude, corrected for sky area of the observations. We have included all point sources within 15.…”

Section: Observations and Reductionsmentioning

confidence: 99%

See 2 more Smart Citations

A Search for Wide Companions to the Extrasolar Planetary System Hr 8799

Males

2009

ApJ

View full text Add to dashboard Cite

The extrasolar planetary system around HR 8799 is the first multiplanet system ever imaged. It is also, by a wide margin, the highest mass system with >27 Jupiters of planetary mass past 25 AU. This is a remarkable system with no analog in any other known planetary system. In the first part of this paper, we investigated the nature of two faint objects imaged near the system. These objects are considerably fainter (H = 20.4 and 21.6 mag) and more distant (projected separations of 612 and 534 AU) than the three known planetary companions b, c, and d (68-24 AU). It is possible that these two objects could be lower mass planets (of mass ∼5M Jup and ∼3M Jup ) that have been scattered to wider orbits. We make the first direct comparison of newly reduced archival Gemini adaptive optics images to archival Hubble Space Telescope/NICMOS images. With nearly a decade between these epochs, we can accurately assess the proper motion nature of each candidate companion. We find that both objects are unbound to HR 8799 and are background. We estimate that HR 8799 has no companions of H < 22 from ∼5 to 15 . Any scattered giant planets in the HR 8799 system are >600 AU or less than 3 M Jup in mass. In the second part of this paper, we search for any sign of a "reverse parallax signature" in the astrometric residuals of HR 8799b. No such signal was found and we conclude, as expected, that HR 8799b has the same parallax as HR 8799A. In the third part of this paper, we carry out a search for wider common proper motion objects. We found one object within 1 deg 2 in the Palomar Observatory Sky Survey-Digitized Sky Survey images with similar (< 2σ ) proper motions to HR 8799 at a separation of 4. 0. We conclude that it is not likely a bound companion to HR 8799 based on available photometry.

show abstract

Section: Are "Hr 8799b" and "Hr 8799c" Background?supporting

confidence: 65%

Section: Observations and Reductionsmentioning

confidence: 99%

Section: Observations and Reductionsmentioning

confidence: 99%

See 1 more Smart Citation

A Search for Wide Companions to the Extrasolar Planetary System Hr 8799

Males

2009

ApJ

View full text Add to dashboard Cite

show abstract

“…A&A 562, A127 (2014) very low-mass objects that would be too faint to study once they have aged were rapidly discovered in young clusters and in young nearby (<100 pc) associations (see the review of Torres et al 2008) during deep infrared surveys (e.g., Robberto et al 2010), observation campaigns with adaptive optics devices (e.g. Chauvin et al 2003Chauvin et al , 2010Ireland et al 2011) and with space observatories (Hubble, Spitzer: e.g Lowrance et al 1999Lowrance et al , 2000Lowrance et al , 2005Luhman et al 2007;Todorov et al 2010). Among these discoveries, planetary mass objects ( 13.6 M Jup , see the definition of the International Astronomical Union) were found to be free-floating (e.g.…”

Section: Introductionmentioning

confidence: 99%

A library of near-infrared integral field spectra of young M–L dwarfs

Bonnefoy

Chauvin

Lagrange

et al. 2014

A&A

142

204

View full text Add to dashboard Cite

Context. At young ages, low surface gravity affects the atmospheric properties of ultracool dwarfs. The impact on medium-resolution near-infrared (NIR) spectra has only been slightly investigated at the M-L transition so far. Aims. We present a library of NIR (1.1-2.45 µm) medium-resolution (R ∼ 1500-2000) integral field spectra of 15 young M6−L0 dwarfs. We aim at deriving updated NIR spectral type, luminosity, and physical parameters (T eff , log g, M, L/L ) for each source. This work also aims at testing the latest generation of BT-SETTL atmospheric models. Methods. We estimated spectral types using spectral indices and the spectra of young objects classified in the optical. We used the 2010 and 2012 releases of the BT-SETTL synthetic spectral grid and cross-checked the results with the DRIFT-PHOENIX models to derive the atmospheric properties of the sources. Results. We do not find significant differences between the spectra of young companions and those of young isolated brown dwarfs in the same spectral type range. We derive infrared spectral types L0 ± 1, L0 ± 1, M9.5 ± 0.5, M9.5 ± 0.5, M9.25 ± 0.25, M8 +0.5 −0.75 , and M8.5 ± 0.5 for AB Pic b, Cha J110913-773444, USco CTIO 108B, GSC 08047-00232 B, DH Tau B, CT Cha b, and HR7329B, respectively. The BT-SETTL and DRIFT-PHOENIX models yield close T eff and log g estimates for each source. The models seem to show a 600 +600 −300 K drop in the effective temperature at the M-L transition. Assuming the former temperatures are correct, we then derive new mass estimates that confirm that DH Tau B, USco CTIO 108B, AB Pic b, KPNO Tau 4, OTS 44, and Cha1109 lie inside or at the boundary of the planetary mass range. We combine the empirical luminosities of the M9.5-L0 sources to the T eff to derive semi-empirical radii estimates that do not match "hot-start" evolutionary models predictions at 1-3 Myr. We use complementary data to demonstrate that atmospheric models are able to reproduce the combined optical and infrared spectral energy distribution, together with the NIR spectra of these sources simultaneously. But the models still fail to represent the dominant features in the optical. This issue raises doubts on the ability of these models to predict effective temperatures from NIR spectra alone. Conclusions. The library provides templates for characterizing other young and late type objects. The study advocates the use of photometric and spectroscopic information over a broad range of wavelengths to study the properties of very low-mass young companions to be detected with the planet imagers (Subaru/SCExAO, LBT/LMIRCam, Gemini/GPI, VLT/SPHERE).

show abstract

“…Direct imaging is a detection method that allows us to characterize large-separation exoplanets. In the past decade many direct imaging surveys (e.g., Lowrance et al 2005;Biller et al 2007;Lafrenière et al 2007;Chauvin et al 2010;Heinze et al 2010;Vigan et al 2012;Biller et al 2013;Rameau et al 2013a;Wahhaj et al 2013;Chauvin et al 2015;Brandt et al 2014a;Bowler et al 2015) have been carried out to evaluate the occurrence of giant planets in wide orbits (10-500 AU).…”

Section: Introductionmentioning

confidence: 99%

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

Reggiani

Meyer

Chauvin

et al. 2016

A&A

View full text Add to dashboard Cite

Context. In recent years there have been many attempts to characterize the occurrence and distribution of stellar, brown dwarf (BD), and planetary-mass companions to solar-type stars with the aim of constraining formation mechanisms. From radial velocity observations a dearth of companions with masses between 10-40 M Jupiter has been noticed at close separations, suggesting the possibility of a distinct formation mechanism for objects above and below this range. Aims. We present a model for the substellar companion mass function (CMF). This model consists of the superposition of the planet and BD companion mass distributions, assuming that we can extrapolate the radial velocity measured CMF for planets to larger separations and the stellar companion mass-ratio distribution over all separations into the BD mass regime. By using both the results of the VLT/NaCo large program (NaCo-LP) and the complementary archive datasets, which probe the occurrence of planets and BDs on wide orbits around solar-type stars, we place some constraints on the planet and BD distributions. Methods. We developed a Monte Carlo simulation tool to predict the outcome of a given survey, depending on the shape of the orbital parameter distributions (mass, semimajor axis, eccentricity, and inclination). Comparing the predictions with the results of the observations, we calculate the likelihood of different models and which models can be ruled out. Results. Current observations are consistent with the proposed model for the CMF, as long as a sufficiently small outer truncation radius ( 100 AU) is introduced for the planet separation distribution. Some regions of parameter space can be excluded by the observations. Conclusions. We conclude that the results of the direct imaging surveys searching for substellar companions around Sun-like stars are consistent with a combined substellar mass spectrum of planets and BDs. This mass distribution has a minimum between 10 and 50 M Jupiter , in agreement with radial velocity measurements. In this picture the dearth of objects in this mass range would naturally arise from the shape of the mass distribution, without the introduction of any distinct formation mechanism for BDs. This kind of model for the CMF allows us to determine the probability for a substellar companion as a function of mass to have formed in a disk or from protostellar core fragmentation, as such mechanisms overlap in this mass range.

show abstract

An Infrared Coronagraphic Survey for Substellar Companions

Cited by 106 publications

References 79 publications

A Search for Wide Companions to the Extrasolar Planetary System Hr 8799

A Search for Wide Companions to the Extrasolar Planetary System Hr 8799

A library of near-infrared integral field spectra of young M–L dwarfs

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

Contact Info

Product

Resources

About