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1801. h and chi Per UBVI,H{alpha} photometry
ID:
ivo://CDS.VizieR/J/AJ/122/248
Title:
h and chi Per UBVI,H{alpha} photometry
Short Name:
J/AJ/122/248
Date:
21 Oct 2021
Publisher:
CDS
Description:
UBVI and H{alpha} photometry is presented for 17319 stars in vicinity of the young double cluster h and {chi} Persei. Our photometry extends over a 37'x1{deg} field centered on the association. We construct reddening contours within the imaged field. We find that the two clusters share a common distance modulus of 11.75+/-0.05 and ages of log[age(yr)]=7.1+/-0.1. From the V-H{alpha} color, a measure of the H{alpha} emission strength, we conduct a survey for emission line objects within the association. We detect a sample of 33 Be stars, eight of which are new detections. We present a scenario of evolutionary enhancement of the Be phenomenon to account for the peak in Be fraction toward the top of the main sequence in the population of h and {chi} Persei and similar young clusters. UBVI and H{alpha} photometry was performed on five nights between 1999 August 17 and 25 at the San Diego State University Mount Laguna Observatory with the 1m telescope and a Loral 2048x2048 CCD.
1802. H and Ks photometry of Trumpler 14
ID:
ivo://CDS.VizieR/J/A+A/515/A26
Title:
H and Ks photometry of Trumpler 14
Short Name:
J/A+A/515/A26
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present adaptive optics (AO) near-infrared observations of the core of the Tr 14 cluster in the Carina region obtained with the ESO multi-conjugate AO demonstrator, MAD. Our campaign yields AO-corrected observations with an image quality of about 0.2' across the 2" field of view, which is the widest AO mosaic ever obtained. We detected almost 2000 sources spanning a dynamic range of 10 mag. The pre-main sequence (PMS) locus in the colour-magnitude diagram is well reproduced by Palla & Stahler isochrones with an age of 3 to 5x10^5^yr, confirming the very young age of the cluster. We derive a very high (deprojected) central density n_0_~4.5(+/-0.5)x10^4^pc^-3^ and estimate the total mass of the cluster to be about ~4.3^+3.3^_-1.5_x10^3^M_{sun}_, although contamination of the field of view might have a significant impact on the derived mass. We show that the pairing process is largely dominated by chance alignment so that physical pairs are difficult to disentangle from spurious ones based on our single epoch observation. Yet, we identify 150 likely bound pairs, 30% of these with a separation smaller than 0.5" (~1300AU). We further show that at the 2{sigma} level massive stars have more companions than lower-mass stars and that those companions are respectively brighter on average, thus more massive. Finally, we find some hints of mass segregation for stars heavier than about 10M_{sun}_. If confirmed, the observed degree of mass segregation could be explained by dynamical evolution, despite the young age of the cluster.
1803. HAPLESS galaxies sample
ID:
ivo://CDS.VizieR/J/MNRAS/452/397
Title:
HAPLESS galaxies sample
Short Name:
J/MNRAS/452/397
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the properties of the first 250 {mu}m blind sample of nearby galaxies (15<D<46Mpc) containing 42 objects from the Herschel Astrophysical Terahertz Large Area Survey. Herschel's sensitivity probes the faint end of the dust luminosity function for the first time, spanning a range of stellar mass (7.4<M*<11.3log10M_{sun}_), star formation activity (-11.8<SSFR<-8.9log10yr^-1^), gas fraction (3-96 per cent), and colour (0.6<FUV-K_S_<7.0mag). The median cold dust temperature is 14.6K, colder than in the Herschel Reference Survey (18.5K) and Planck Early Release Compact Source Catalogue (17.7K). The mean dust-to-stellar mass ratio in our sample is higher than these surveys by factors of 3.7 and 1.8, with a dust mass volume density of (3.7+/-0.7)x10^5^M_{sun}_/Mpc^3^. Counter-intuitively, we find that the more dust rich a galaxy, the lower its UV attenuation. Over half of our dust-selected sample are very blue in FUV-K_S_ colour, with irregular and/or highly flocculent morphology; these galaxies account for only 6 per cent of the sample's stellar mass but contain over 35 per cent of the dust mass. They are the most actively star-forming galaxies in the sample, with the highest gas fractions and lowest UV attenuation. They also appear to be in an early stage of converting their gas into stars, providing valuable insights into the chemical evolution of young galaxies.
1804. HAQ survey: red QSO candidates follow-up
ID:
ivo://CDS.VizieR/J/ApJS/217/5
Title:
HAQ survey: red QSO candidates follow-up
Short Name:
J/ApJS/217/5
Date:
21 Oct 2021
Publisher:
CDS
Description:
Quasi-stellar objects (QSOs) whose spectral energy distributions (SEDs) are reddened by dust either in their host galaxies or in intervening absorber galaxies are to a large degree missed by optical color selection criteria like the ones used by the Sloan Digital Sky Survey (SDSS). To overcome this bias against red QSOs, we employ a combined optical and near-infrared (near-IR) color selection. In this paper, we present a spectroscopic follow-up campaign of a sample of red candidate QSOs which were selected from the SDSS and the UKIRT Infrared Deep Sky Survey (UKIDSS). The spectroscopic data and SDSS/UKIDSS photometry are supplemented by mid-infrared photometry from the Wide-field Infrared Survey Explorer. In our sample of 159 candidates, 154 (97%) are confirmed to be QSOs. We use a statistical algorithm to identify sightlines with plausible intervening absorption systems and identify nine such cases assuming dust in the absorber similar to Large Magellanic Cloud sightlines. We find absorption systems toward 30 QSOs, 2 of which are consistent with the best-fit absorber redshift from the statistical modeling. Furthermore, we observe a broad range in SED properties of the QSOs as probed by the rest-frame 2{mu}m flux. We find QSOs with a strong excess as well as QSOs with a large deficit at rest-frame 2{mu}m relative to a QSO template. Potential solutions to these discrepancies are discussed. Overall, our study demonstrates the high efficiency of the optical/near-IR selection of red QSOs.
1805. HATLAS candidate lensed galaxies
ID:
ivo://CDS.VizieR/J/MNRAS/465/3558
Title:
HATLAS candidate lensed galaxies
Short Name:
J/MNRAS/465/3558
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a sample of 80 candidate strongly lensed galaxies with flux density above 100mJy at 500{mu}m extracted from the Herschel Astrophysical Terahertz Large Area Survey, over an area of 600deg^2^. Available imaging and spectroscopic data allow us to confirm the strong lensing in 20 cases and to reject it in one case. For other eight objects, the lensing scenario is strongly supported by the presence of two sources along the same line of sight with distinct photometric redshifts. The remaining objects await more follow-up observations to confirm their nature. The lenses and the background sources have median redshifts z_L_=0.6 and z_S_=2.5, respectively, and are observed out to z_L_=1.2 and z_S_=4.2. We measure the number counts of candidate lensed galaxies at 500{mu}m and compare them with theoretical predictions, finding a good agreement for a maximum magnification of the background sources in the range 10-20. These values are consistent with the magnification factors derived from the lens modelling of individual systems. The catalogue presented here provides sub-mm bright targets for follow-up observations aimed at exploiting gravitational lensing, to study with unprecedented details the morphological and dynamical properties of dusty star-forming regions in z>=1.5 galaxies.
1806. H-ATLAS search for strongly lensed galaxies
ID:
ivo://CDS.VizieR/J/ApJ/749/65
Title:
H-ATLAS search for strongly lensed galaxies
Short Name:
J/ApJ/749/65
Date:
21 Oct 2021
Publisher:
CDS
Description:
While the selection of strongly lensed galaxies (SLGs) with 500{mu}m flux density S_500_>100mJy has proven to be rather straightforward, for many applications it is important to analyze samples larger than the ones obtained when confining ourselves to such a bright limit. Moreover, only by probing to fainter flux densities is it possible to exploit strong lensing to investigate the bulk of the high-z star-forming galaxy population. We describe HALOS (the Herschel-ATLAS Lensed Objects Selection), a method for efficiently selecting fainter candidate SLGs, reaching a surface density of =~1.5-2/deg^2^, i.e., a factor of about 4-6 higher than that at the 100mJy flux limit. HALOS will allow the selection of up to ~1000 candidate SLGs (with amplifications {mu}>~2) over the full H-ATLAS survey area. Applying HALOS to the H-ATLAS Science Demonstration Phase field (=~14.4deg^2^) we find 31 candidate SLGs, whose candidate lenses are identified in the VIKING near-infrared catalog. Using the available information on candidate sources and candidate lenses we tentatively estimate a =~72% purity of the sample. As expected, the purity decreases with decreasing flux density of the sources and with increasing angular separation between candidate sources and lenses. The redshift distribution of the candidate lensed sources is close to that reported for most previous surveys for lensed galaxies, while that of candidate lenses extends to redshifts substantially higher than found in the other surveys. The counts of candidate SLGs are also in good agreement with model predictions. Even though a key ingredient of the method is the deep near-infrared VIKING photometry, we show that H-ATLAS data alone allow the selection of a similarly deep sample of candidate SLGs with an efficiency close to 50%; a slightly lower surface density (=~ 1.45/deg2) can be reached with a ~70% efficiency.
1807. HATNet Pleiades Rotation Period Catalogue
ID:
ivo://CDS.VizieR/J/MNRAS/408/475
Title:
HATNet Pleiades Rotation Period Catalogue
Short Name:
J/MNRAS/408/475
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using data from the Hungarian-made Automated Telescope Network (HATNet) survey for transiting exoplanets, we measure photometric rotation periods for 368 Pleiades stars with 0.4~<M~<1.3M_{sun}_. We detect periodic variability for 74 per cent of the cluster members in this mass range that are within our field-of-view, and 93 per cent of the members with 0.7~<M~<1.0M_{sun}_. This increases, by a factor of 5, the number of Pleiades members with measured periods. We compare these data to the rich sample of spectroscopically determined projected equatorial rotation velocities (vsini) available in the literature for this cluster. Included in our sample are 14 newly identified probable cluster members which have proper motions, photometry and rotation periods consistent with membership.
1808. HATNET variability survey
ID:
ivo://CDS.VizieR/J/AJ/128/1761
Title:
HATNET variability survey
Short Name:
J/AJ/128/1761
Date:
21 Oct 2021
Publisher:
CDS
Description:
The Hungarian-made Automated Telescope Network (HATnet) is an ongoing project to detect transiting extrasolar planets using small-aperture (11cm diameter) robotic telescopes. In this paper, we present the results from using image subtraction photometry to reduce a crowded stellar field observed with one of the HATnet telescopes (HAT-5). This field was chosen to overlap with the planned Kepler mission. We obtained I-band light curves for 98,000 objects in a 67 square degree field of view centered at J2000 ({alpha},{delta})=(19h44m00.0s, +37{deg}32'00.0"), near the Galactic plane in the constellations Cygnus and Lyra. These observations include 788 exposures of 5' length over 30-days. For the brightest stars (I~8.0) we achieved a precision of 3.5mmag, falling to 0.1mag at the faint end (I~14). From these light curves we identify 1617 variable stars, of which 1439 are newly discovered.
1809. HAT-P-44, HAT-P-45, and HAT-P-46 follow-up
ID:
ivo://CDS.VizieR/J/AJ/147/128
Title:
HAT-P-44, HAT-P-45, and HAT-P-46 follow-up
Short Name:
J/AJ/147/128
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery by the HATNet survey of three new transiting extrasolar planets orbiting moderately bright (V=13.2, 12.8, and 11.9) stars. The planets have orbital periods of 4.3012, 3.1290, and 4.4631 days, masses of 0.35, 0.89, and 0.49M_J_, and radii of 1.24, 1.43, and 1.28R_J_. The stellar hosts have masses of 0.94, 1.26, and 1.28M_{sun}_. Each system shows significant systematic variations in its residual radial velocities, indicating the possible presence of additional components. Based on its Bayesian evidence, the preferred model for HAT-P-44 consists of two planets, including the transiting component, with the outer planet having a period of 872 days, eccentricity of 0.494+/-0.081, and a minimum mass of 4.0M_J_. Due to aliasing we cannot rule out alternative solutions for the outer planet having a period of 220 days or 438 days. For HAT-P-45, at present there is not enough data to justify the additional free parameters included in a multi-planet model; in this case a single-planet solution is preferred, but the required jitter of 22.5+/-6.3m/s is relatively high for a star of this type. For HAT-P-46 the preferred solution includes a second planet having a period of 78 days and a minimum mass of 2.0M_J_, however the preference for this model over a single-planet model is not very strong. While substantial uncertainties remain as to the presence and/or properties of the outer planetary companions in these systems, the inner transiting planets are well characterized with measured properties that are fairly robust against changes in the assumed models for the outer planets. Continued radial velocity monitoring is necessary to fully characterize these three planetary systems, the properties of which may have important implications for understanding the formation of hot Jupiters.
1810. HATS-39b, 40b, 41b and 42b transit data
ID:
ivo://CDS.VizieR/J/MNRAS/477/3406
Title:
HATS-39b, 40b, 41b and 42b transit data
Short Name:
J/MNRAS/477/3406
Date:
04 Feb 2022 06:26:57
Publisher:
CDS
Description:
We report the discovery of four transiting hot Jupiters from the HATSouth survey: HATS-39b, HATS-40b, HATS-41b, and HATS-42b. These discoveries add to the growing number of transiting planets orbiting moderately bright (12.5<=V<=13.7) F dwarf stars on short (2-5d) periods. The planets have similar radii, ranging from 1.33^+0.29^_-0.20_R_J_ for HATS-41b to 1.58^+0.16^_-0.12_R_J_ for HATS-40b. Their masses and bulk densities, however, span more than an order of magnitude. HATS-39b has a mass of 0.63+/-0.13M_J_, and an inflated radius of 1.57+/-0.12R_J_, making it a good target for future transmission spectroscopic studies. HATS-41b is a very massive 9.7+/-1.6M_J_ planet and one of only a few hot Jupiters found to date with a mass over 5M_J_. This planet orbits the highest metallicity star ([Fe/H]=0.470+/-0.010) known to host a transiting planet and is also likely on an eccentric orbit. The high mass, coupled with a relatively young age (1.34^+0.31^_-0.51_Gyr) for the host star, is a factor that may explain why this planet's orbit has not yet circularized.