- ID:
- ivo://CDS.VizieR/J/AJ/120/2747
- Title:
- HDF-South WFPC2 observations
- Short Name:
- J/AJ/120/2747
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z>2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.
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2492. HDF-S: STIS imaging
- ID:
- ivo://CDS.VizieR/J/AJ/119/486
- Title:
- HDF-S: STIS imaging
- Short Name:
- J/AJ/119/486
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.
- ID:
- ivo://CDS.VizieR/J/A+A/347/164
- Title:
- HD 59435 Geneva photometry
- Short Name:
- J/A+A/347/164
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The SB2 binary HD 59435 hosts a yellow giant and a magnetic Ap star, the latter being the secondary (Wade et al., 1996, Cat. <J/A+A/314/491>) and exhibiting spectral lines resolved into their magnetically-split components. Additional measurements of the magnetic field modulus of the Ap secondary are reported, as well as additional radial velocities for both components and photometric magnitudes and colours in the Geneva system. The magnetic field modulus varies with a period of about 1360 days. For a general description of the Geneva photometric system, see e.g. <GCPD/13>
- ID:
- ivo://CDS.VizieR/J/A+A/629/A75
- Title:
- HD 97048 H13CO+ and HC15N first detections
- Short Name:
- J/A+A/629/A75
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Observations of different molecular lines in protoplanetary disks provide valuable information on the gas kinematics, as well as constraints on the radial density and temperature structure of the gas. With ALMA we have detected H13CO+ (J=4-3) and HC15N (J=4-3) in the HD 97048 protoplanetary disk for the first time. We compare these new detections to the ringed continuum mm-dust emission and the spatially resolved CO (J=3-2) and HCO+ (J=4-3) emission. The radial distributions of the H^13^CO^+^ and HC^15^N emission show hints of ringed sub-structure whereas, the optically thick tracers, CO and HCO+, do not. We calculate the HCO^+^/H^13^CO^+^ intensity ratio across the disk and find that it is radially constant (within our uncertainties). We use a physio-chemical parametric disk structure of the HD 97048 disk with an analytical prescription for the HCO^+^ abundance distribution to generate synthetic observations of the HCO^+^ and H^13^CO^+^ disk emission assuming LTE. The best by-eye fit models require radial variations in the HCO^+^/H^13^CO^+^ abundance ratio and an overall enhancement in H^13^CO^+^ relative to HCO^+^. This highlights the need to consider isotope selective chemistry and in particular low temperature carbon isotope exchange reactions. This also points to the presence of a reservoir of cold molecular gas in the outer disk (T<10K, R>200au). Chemical models are required to confirm that isotope-selective chemistry alone can explain the observations presented here. With these data, we cannot rule out that the known dust substructure in the HD 97048 disk is responsible for the observed trends in molecular line emission, and higher spatial resolution observations are required to fully explore the potential of optically thin tracers to probe planet-carved dust gaps. We also report non-detections of H^13^CO^+^ and HC^15^N in the HD 100546 protoplanetary disk.
- ID:
- ivo://CDS.VizieR/J/A+A/626/A95
- Title:
- HD160305 images with SPHERE
- Short Name:
- J/A+A/626/A95
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Direct imaging of debris disks gives important information about their nature, their global morphology and allows to identify specific structures possibly in connection with the presence of gravitational perturbers. It is the most straightforward technique to observe planetary systems as a whole. We present the first resolved images of the debris disk around the young F-type star HD 160305, detected in scattered light using the VLT/SPHERE instrument in the near infrared. We used a post-processing method based on Angular Differential Imaging and synthetic images of debris disks produced with a disk modeling code (GRaTer) to constrain the main characteristics of the disk around HD160305. All of the point sources in the field of the IRDIS camera were analyzed with an astrometric tool to determine whether they are bound objects or background stars. We detect a very inclined (~82{deg}) ring-like debris disk located at a stellocentric distance of about 86au (deprojected width ~27au). The disk displays a brightness asymmetry between the two sides of the major axis, as can be expected from scattering properties of dust grains. We derive an anisotropic scattering factor g>0.5. A second right-left asymmetry is also observed with respect to the minor axis. We measure a surface brightness ratio of 0.73+/-0.18 between the bright and the faint sides. Because of the low signal-to-noise ratio (S/N) of the images we cannot easily discriminate between several possible explanations for this left-right asymmetry, such as perturbations by an unseen planet, the aftermath of the breakup of a massive planetesimal, or the pericenter glow effect due to an eccentric ring. Two epochs of observations allow us to reject the companionship hypothesis for the 15 point sources present in the field.
- ID:
- ivo://CDS.VizieR/J/A+A/635/A6
- Title:
- HD 219134 light and RV curves and code
- Short Name:
- J/A+A/635/A6
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- By analysing the transit light-curve of a planet-hosting star or the induced radial velocity oscillations, many useful information on the planet may be retrieved. However, inferring the physical parameters of the planet (mass, size, semi-major axis, etc.) requires the preliminary knowledge of some parameters of the host star, especially its mass and/or radius, that are generally inferred through theoretical evolutionary models. The paper aims at presenting and testing a whole algorithm devoted to the complete characterization of an exoplanetary system thanks to the global analysis of photometric and/or radial velocity time-series combined to observational stellar parameters derived either from spectroscopy or photometry. We developed an integrated tool called MCMCI that combines the Markov Chain Monte Carlo (MCMC) approach for analysing photometric and/or radial velocity time-series with a proper interpolation within stellar evolutionary isochrones and tracks (known as Isochrone placement) to be performed at each chain step, to retrieve stellar theoretical parameters, such as age, mass and radius. We tested the MCMCI both on the HD 219134 multiplanetary system hosting two transiting rocky super-Earths and on WASP-4, that hosts a bloated hot Jupiter. Even considering different input approaches, a final convergence was reached within the code, we found good agreement with the results already stated in the literature and we obtained more precise output parameters, especially concerning planetary masses. The MCMCI tool offers the opportunity of performing an integrated analysis of an exoplanetary system, without splitting it into the preliminary stellar characterization through theoretical models, but rather favouring a close interaction between the light-curve analysis and the isochrones, so that the parameters recovered at each step of the MCMC enter as input of the Isochrone placement.
- ID:
- ivo://CDS.VizieR/J/A+A/645/A25
- Title:
- HD27130 photometric light curves
- Short Name:
- J/A+A/645/A25
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The derivation of accurate and precise masses and radii is possible for eclipsing binary stars, allowing for insights into their evolution. When residing in star clusters, they provide measurements of even greater precision, along with additional information on their properties. Asteroseismic investigations of solar-like oscillations offers similar possibilities for single stars. We wish to improve the previously established properties of the Hyades eclipsing binary HD 27130 and re-assess the asteroseismic properties of the giant star {epsilon} Tau. The physical properties of these members of the Hyades can be used to constrain the helium content and age of the cluster. New multi-colour light curves were combined with multi-epoch radial velocities to yield masses and radii of HD 27130. Measurements of Teff were derived from spectroscopy and photometry, and verified using the Gaia parallax. We estimated the cluster age from re-evaluated asteroseismic properties of {epsilon} Tau while using HD 27130 to constrain the helium content. The masses, radii, and Teff of HD 27130 were found to be M=1.0245+/-0.0024M_{sun}_, R=0.9226+/-0.015R_{sun}_, Teff=5650+/-50K for the primary, and M=0.7426+/-0.0016M_{sun}_, R=0.7388+/-0.026R_{sun}_, Teff=4300+/-100K for the secondary component. Our re-evaluation of {epsilon} Tau suggests that the previous literature estimates are trustworthy and that the HIPPARCOS parallax is more reliable than the Gaia DR2 parallax. The helium content of HD 27130 and, thus, of the Hyades is found to be Y=0.27 but with a significant model dependency. Correlations with the adopted metallicity result in a robust helium enrichment law, with {DELTA}Y/{DELTA}Z close to 1.2 We estimate the age of the Hyades to be 0.9+/-0.1(stat)+/-0.1(sys)Gyr, which is in slight tension with recent age estimates based on the cluster white dwarfs. The precision of the age estimate can be much improved via asteroseismic investigations of the other Hyades giants and by future improvements to the Gaia parallax for bright stars.
- ID:
- ivo://CDS.VizieR/J/ApJ/761/46
- Title:
- HD 37605 radial velocities and photometry
- Short Name:
- J/ApJ/761/46
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the radial velocity discovery of a second planetary mass companion to the K0 V star HD 37605, which was already known to host an eccentric, P~55 days Jovian planet, HD 37605b. This second planet, HD 37605c, has a period of ~7.5 years with a low eccentricity and an Msini of ~3.4M_Jup_. Our discovery was made with the nearly 8 years of radial velocity follow-up at the Hobby-Eberly Telescope and Keck Observatory, including observations made as part of the Transit Ephemeris Refinement and Monitoring Survey effort to provide precise ephemerides to long-period planets for transit follow-up. With a total of 137 radial velocity observations covering almost 8 years, we provide a good orbital solution of the HD 37605 system, and a precise transit ephemeris for HD 37605b. Our dynamic analysis reveals very minimal planet-planet interaction and an insignificant transit time variation. Using the predicted ephemeris, we performed a transit search for HD 37605b with the photometric data taken by the T12 0.8m Automatic Photoelectric Telescope (APT) and the MOST satellite. Though the APT photometry did not capture the transit window, it characterized the stellar activity of HD 37605, which is consistent of it being an old, inactive star, with a tentative rotation period of 57.67 days. The MOST photometry enabled us to report a dispositive null detection of a non-grazing transit for this planet. Within the predicted transit window, we exclude an edge-on predicted depth of 1.9% at the {Gt}10{sigma} level, and exclude any transit with an impact parameter b>0.951 at greater than 5{sigma}. We present the BOOTTRAN package for calculating Keplerian orbital parameter uncertainties via bootstrapping. We made a comparison and found consistency between our orbital fit parameters calculated by the RVLIN package and error bars by BOOTTRAN with those produced by a Bayesian analysis using MCMC.
- ID:
- ivo://CDS.VizieR/J/ApJ/754/37
- Title:
- HD 192263 radial velocities and photometry
- Short Name:
- J/ApJ/754/37
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- As part of the Transit Ephemeris Refinement and Monitoring Survey, we present new radial velocities and photometry of the HD 192263 system. Our analysis of the already available Keck-HIRES and CORALIE radial velocity measurements together with the five new Keck measurements we report in this paper results in improved orbital parameters for the system. We derive constraints on the size and phase location of the transit window for HD 192263b, a Jupiter-mass planet with a period of 24.3587+/-0.0022 days. We use 10 years of Automated Photoelectric Telescope photometry to analyze the stellar variability and search for planetary transits. We find continuing evidence of spot activity with periods near 23.4 days. The shape of the corresponding photometric variations changes over time, giving rise to not one but several Fourier peaks near this value. However, none of these frequencies coincides with the planet's orbital period and thus we find no evidence of star-planet interactions in the system. We attribute the ~23 day variability to stellar rotation. There are also indications of spot variations on longer (8 years) timescales. Finally, we use the photometric data to exclude transits for a planet with the predicted radius of 1.09R_J_, and as small as 0.79R_J_.
- ID:
- ivo://CDS.VizieR/J/AJ/132/1910
- Title:
- HD 131861 radial velocities and VRI light curves
- Short Name:
- J/AJ/132/1910
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Our red-wavelength spectroscopic observations of HD 131861, a previously known single-line multiple system, span 20 years. Now lines of two components, the short-period F5 V primary and G8 V secondary, have been detected. The inner orbit is circular with a period of 3.5507439-days, while the outer orbit of the system has a period of 1642 days or 4.496-yr and a relatively low eccentricity of 0.10. Analysis of the Hipparcos data produces a well-determined astrometric orbit for the long-period system that has an inclination of 52{deg}. Our photometric observations show shallow primary and secondary eclipses of the short-period pair, and eclipse solutions result in an inclination of 81{deg}. Thus, the long- and short-period orbits are not coplanar. The mass of the unseen third component is 0.7M_{dot}_, corresponding to a mid-K dwarf. The total mass of the system, 3.08M_{dot}_, leads to a semimajor axis of 4AU for the outer orbit. The F5 V primary is rotating more slowly than it would if it were synchronously rotating, while the G8 V secondary may be synchronously rotating. The lithium abundance of the F5 V primary is similar to the initial lithium abundance found for Population I dwarfs and so indicates no significant dilution.
