A synthetic view on structure and evolution of the Milky Way

Robin, A. C.; Reylé, C.; Derriére, S.; Picaud, S.

doi:10.1051/0004-6361:20031117

Cited by 1,951 publications

(2,550 citation statements)

References 101 publications

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“…We used the Besançon model (Robin et al 2003) to determine the probability of a stellar contaminant close to 51 Peg, whose spectrum would cause the magnitude of the observed signal. Given the area of the CCF for the (here suggested) planetary signal (10 −4 ) and the magnitude of 51 Peg, the contaminant should be of magnitude 16 or brighter (brighter if the contaminant does not fall entirely within the HARPS fibre, which has a diameter of 1 arcsec).…”

Section: Discussionmentioning

confidence: 99%

Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b

Martins

Santos

Figueira

et al. 2015

A&A

133

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Context. The detection of reflected light from an exoplanet is a difficult technical challenge at optical wavelengths. Even though this signal is expected to replicate the stellar signal, not only is it several orders of magnitude fainter, but it is also hidden among the stellar noise. Aims. We apply a variant of the cross-correlation technique to HARPS observations of 51 Peg to detect the reflected signal from planet 51 Peg b. Methods. Our method makes use of the cross-correlation function (CCF) of a binary mask with high-resolution spectra to amplify the minute planetary signal that is present in the spectra by a factor proportional to the number of spectral lines when performing the cross correlation. The resulting cross-correlation functions are then normalized by a stellar template to remove the stellar signal. Carefully selected sections of the resulting normalized CCFs are stacked to increase the planetary signal further. The recovered signal allows probing several of the planetary properties, including its real mass and albedo. Results. We detect evidence for the reflected signal from planet 51 Peg b at a significance of 3σ noise . The detection of the signal permits us to infer a real mass of 0.46 +0.06 −0.01 M Jup (assuming a stellar mass of 1.04 M Sun ) for the planet and an orbital inclination of 80 +10 −19 degrees. The analysis of the data also allows us to infer a tentative value for the (radius-dependent) geometric albedo of the planet. The results suggest that 51Peg b may be an inflated hot Jupiter with a high albedo (e.g., an albedo of 0.5 yields a radius of 1.9 ± 0.3 R Jup for a signal amplitude of 6.0 ± 0.4 × 10 −5 ). Conclusions. We confirm that the method we perfected can be used to retrieve an exoplanet's reflected signal, even with current observing facilities. The advent of next generation of instruments (e.g. VLT-ESO/ESPRESSO) and observing facilities (e.g. a new generation of ELT telescopes) will yield new opportunities for this type of technique to probe deeper into exoplanets and their atmospheres.

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Section: Discussionmentioning

confidence: 99%

Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b

Martins

Santos

Figueira

et al. 2015

A&A

133

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“…For another dark cloud of the complex (LDN 1439, CB 26), Launhardt & Sargent (2001) adopted a distance of 140 pc based on a re-examination of the larger-scale velocity structure. An upper limit to the distance of LDN 1415 can be derived using the stellar population model of the Galaxy of Robin et al (2003).…”

Section: The Distance To Ldn 1415mentioning

confidence: 99%

The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Stecklum¹,

Melnikov

Meusinger³

2006

A&A

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Aims.A survey for candidate Herbig-Haro objects was performed to search for evidence of star formation in Galactic dark clouds Methods. For this aim true colour images were created from blue, red, and infrared DSS2 plates and inspected. Follow-up I-band, Hα, and [S ii] CCD imaging as well as long-slit spectroscopy using the Tautenburg 2-m telescope was carried out to verify candidate objects.Results. In the case of LDN 1415, the presence of a Herbig-Haro flow could be revealed which is henceforth named HH 892. In addition, an arcuate nebula was found which is barely seen on the DSS2 infrared plate (epoch 1996) and not detected in archival Kiso Schmidt data (epoch 2001). Thus, this nebula must have brightened by about 3.8 mag in recent years. Conclusions. The nebula is associated with IRAS 04376+5413. The 2MASS images show a red counterpart of the IRAS source, designated as L1415-IRS. Its morphology resembles that of a bipolar young object. The luminosity of this source integrated from 0.9 µm to 60 µm in the low state amounts to 0.13 L for an assumed distance of 170 pc. Thus it seems to be a young very-low mass star or it might even be of substellar mass. The current brightness increase of the nebula is caused by a FUor-or EXor-like outburst as indicated by the presence of a P Cygni profile of the Hα line. L1415-IRS is by far the least luminous member of the sparse sample of FUor and EXor objects.

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“…The median V magnitude of the HAT planethost stars is nearly a magnitude brighter than the WASP median. Experiments with the Besançon galactic model (Robin et al 2003) show that, at the intermediate galactic latitudes where these surveys are conducted, stars of luminosity class V show a steady decrease in median metallicity with increasing V magnitude. Although this trend is not in itself sufficient to explain the difference in the two samples, metal-poor stars of a given I magnitude also appear brighter in the WASP cameras owing to their lower line blanketing.…”

Section: Survey Strategies and System Propertiesmentioning

confidence: 99%

Statistical patterns in ground-based transit surveys

Cameron

2010

Proc. IAU

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Abstract. As the number of known transiting planets from ground-based surveys passes the 100 mark, it is becoming possible to perform meaningful statistical analyses on their physical properties. Caution is needed in their interpretation, because subtle differences in survey strategy can lead to surprising selection effects affecting the distributions of planetary orbital periods and radii, and of host-star metallicity. Despite these difficulties, the planetary mass-radius relation appears to conform more or less to theoretical expectations in the mass range from Saturns to super-Jupiters. The inflated radii of many hot Jupiters indicate that environmental factors can have a dramatic effect on planetary structure, and may even lead to catastrophic loss of the planetary envelope under extreme irradiation. High-precision radial velocities and secondaryeclipse timing are yielding eccentricity measurements of exquisite precision. They show some hot Jupiters to be in almost perfectly circular orbits, while others remain slightly but significantly eccentric.

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A synthetic view on structure and evolution of the Milky Way

Cited by 1,951 publications

References 101 publications

Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b

Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b

The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Statistical patterns in ground-based transit surveys

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