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811. Alignment of galaxies in galaxy clusters
ID:
ivo://CDS.VizieR/J/A+A/575/A48
Title:
Alignment of galaxies in galaxy clusters
Short Name:
J/A+A/575/A48
Date:
21 Oct 2021
Publisher:
CDS
Description:
Torques acting on galaxies lead to physical alignments, but the resulting ellipticity correlations are difficult to predict. As they constitute a major contaminant for cosmic shear studies, it is important to constrain the intrinsic alignment signal observationally. We measured the alignments of satellite galaxies within 90 massive galaxy clusters in the redshift range 0.05<z<0.55 and quantified their impact on the cosmic shear signal. We combined a sample of 38104 galaxies with spectroscopic redshifts with high-quality data from the Canada-France-Hawaii Telescope. We used phase-space information to select 14576 cluster members, 14250 of which have shape measurements and measured three different types of alignment: the radial alignment of satellite galaxies toward the brightest cluster galaxies (BCGs), the common orientations of satellite galaxies and BCGs, and the radial alignments of satellites with each other. Residual systematic effects are much smaller than the statistical uncertainties. We detect no galaxy alignment of any kind out to at least 3r_200_. The signal is consistent with zero for both blue and red galaxies, bright and faint ones, and also for subsamples of clusters based on redshift, dynamical mass, and dynamical state. These conclusions are unchanged if we expand the sample with bright cluster members from the red sequence. We augment our constraints with those from the literature to estimate the importance of the intrinsic alignments of satellites compared to those of central galaxies, for which the alignments are described by the linear alignment model. Comparison of the alignment signals to the expected uncertainties of current surveys such as the Kilo-Degree Survey suggests that the linear alignment model is an adequate treatment of intrinsic alignments, but it is not clear whether this will be the case for larger surveys.
812. Alignments of quasar polarization vectors
ID:
ivo://CDS.VizieR/J/A+A/441/915
Title:
Alignments of quasar polarization vectors
Short Name:
J/A+A/441/915
Date:
21 Oct 2021
Publisher:
CDS
Description:
Based on a new sample of 355 quasars with significant optical polarization and using complementary statistical methods, we confirm that quasar polarization vectors are not randomly oriented over the sky with a probability often in excess of 99.9%.
813. A list of ~330000 stars Kepler missed
ID:
ivo://CDS.VizieR/J/AJ/161/231
Title:
A list of ~330000 stars Kepler missed
Short Name:
J/AJ/161/231
Date:
09 Mar 2022 22:00:00
Publisher:
CDS
Description:
The Kepler Mission revolutionized exoplanet science and stellar astrophysics by obtaining highly precise photometry of over 200000 stars over 4yr. A critical piece of information to exploit Kepler data is its selection function, since all targets had to be selected from a sample of half a million stars on the Kepler CCDs using limited information. Here we use Gaia DR2 to reconstruct the Kepler selection function and explore possible biases with respect to evolutionary state, stellar multiplicity, and kinematics. We find that the Kepler target selection is nearly complete for stars brighter than Kp<14mag and was effective at selecting main-sequence stars, with the fraction of observed stars decreasing from 95% to 60% between 14<Kp<16mag. We find that the observed fraction for subgiant stars is only 10% lower, confirming that a significant number of subgiants selected for observation were believed to be main-sequence stars. Conversely we find a strong selection bias against low-luminosity red giant stars (R~3-5R_{sun}_, Teff~5500K), dropping from 90% at Kp=14mag to below 30% at Kp=16mag, confirming that the target selection was efficient at distinguishing dwarfs from giants. We compare the Gaia Re-normalized Unit Weight Error (RUWE) values of the observed and nonobserved main-sequence stars and find a difference in elevated (>1.2) RUWE values at ~{sigma} significance, suggesting that the Kepler target selection shows some bias against either close or wide binaries. We furthermore use the Gaia proper motions to show that the Kepler selection function was unbiased with respect to kinematics.
814. A list of Supergiant Stars
ID:
ivo://CDS.VizieR/V/17A
Title:
A list of Supergiant Stars
Short Name:
V/17A
Date:
21 Oct 2021
Publisher:
CDS
Description:
This catalogue is a compilation of about 5000 stars classified as supergiants (class I or II) in the literature. The following information is given: DM and HD identifications, coordinates, photometry, radial velocity and MK classification
815. A list of tantalum lines
ID:
ivo://CDS.VizieR/J/AZh/92/834
Title:
A list of tantalum lines
Short Name:
J/AZh/92/834
Date:
21 Oct 2021
Publisher:
CDS
Description:
The list contains wavelengths of spectral lines of neutral and single ionized tantalum for accurate calibration of the Hamilton echelle spectrograph installed at the Shane 3-m telescope of the Lick observatory that was in operation before June 9, 2011 (S&J Box, Westinghouse WL23418, symbol ThAr02). Furthermore, the list may be used for wavelength calibration of another Lick lamp (symbol ThAr07, Westinghouse Box, Westinghouse WL32809) that was in operation from February 17, 1995 to June 19, 2011.
816. Allard, COND 2000
ID:
ivo://svo.cab/models/cond00
Title:
Allard, COND 2000
Short Name:
COND00
Date:
04 Sep 2019 08:27:24
Publisher:
SVO CAB
Description:
The COND00 Model grid of theoretical spectra (Lyon group)
817. Allard, DUSTY 2000
ID:
ivo://svo.cab/models/dusty00
Title:
Allard, DUSTY 2000
Short Name:
DUSTY00
Date:
04 Sep 2019 08:28:21
Publisher:
SVO CAB
Description:
The DUSTY00 Model grid of theoretical spectra (Lyon group)
818. Allen Telescope Array Pi GHz Sky Survey (PiGSS) Boo Field Source Catalog
ID:
ivo://nasa.heasarc/pigssboofd
Title:
Allen Telescope Array Pi GHz Sky Survey (PiGSS) Boo Field Source Catalog
Short Name:
PIGSSBOOFD
Date:
28 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Pi GHz Sky Survey (PiGSS) is a key project of the Allen Telescope Array (ATA). PiGSS is a 3.1 GHz survey of radio continuum emission in the extragalactic sky with an emphasis on synoptic observations that measure the static and time-variable properties of the sky. During the 2.5 year campaign, PiGSS will twice observe ~250,000 radio sources in the 10,000 deg&lt;sup&gt;2&lt;/sup&gt; region of the sky with b &gt; 30 degrees to an rms sensitivity of ~1 mJy. Additionally, sub-regions of the sky will be observed multiple times to characterize variability on timescales of days to years. Presented here are the results from observations of a 10 deg&lt;sup&gt;2&lt;/sup&gt; region in the Bootes constellation overlapping the NOAO Deep Wide Field Survey field. The PiGSS image was constructed from 75 daily observations distributed over a 4 month period and has an rms flux density between 200 and 250 &micro;Jy. This represents a deeper image by a factor of 4-8 than the authors will achieve over the entire 10,000 deg&lt;sup&gt;2&lt;/sup&gt;. In this table, they provide flux densities, source sizes, and spectral indices for the 425 sources detected in the image. They identify ~100 new flat-spectrum radio sources, and project that, when completed, PiGSS will identify 104 flat-spectrum sources. In their paper the authors identify one source that is a possible transient radio source. This survey provides new limits on faint radio transients and variables with characteristic durations of months. This table was created by the HEASARC in March 2011 based on electronic versions of Tables 2 and 4 from the reference paper which were obtained from the ApJ web site. The HEASARC changed the sign of the values of the last parameter in Table 4 (herein called spectral_index_3_error) from negative to positive. In March 2013, after receiving a clarification from Steve Croft, the HEASARC corrected the names of the 4 parameters describing the source sizes (to reflect the fact that they were diameters nor radii) to major_axis, minor_axis, fit_major_axis and fit_minor_axis. This is a service provided by NASA HEASARC .
819. Allen Telescope Array Pi GHz Sky Survey (PiGSS) Deep Fields Source Catalog
ID:
ivo://nasa.heasarc/pigsselcnf
Title:
Allen Telescope Array Pi GHz Sky Survey (PiGSS) Deep Fields Source Catalog
Short Name:
PIGSSELCNF
Date:
28 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains results from a total of 459 repeated 3.1-GHz radio continuum observations (of which 379 were used in a search for transient sources) of the ELAIS-N1, Coma, Lockman Hole, and NOAO Deep Wide Field Survey (NDWFS) fields as part of the Allen Telescope Array (ATA) Pi GHz Sky Survey (PiGSS). The observations were taken in 2 simultaneous 100-MHz wide bands centered at 3.04 and 3.14 GHz approximately once per day between 2009 May and 2011 April. Each image covers 11.8 square degrees and has 100&quot; FWHM resolution. Deep images for each of the four fields have rms noise between 180 and 310 &micro;Jy (&micro;Jy), and the corresponding catalogs contain ~200 sources in each field. Typically 40-50 of these sources are detected in each single-epoch image. This represents one of the shortest cadence, largest area, multi-epoch surveys undertaken at these frequencies. The authors compared the catalogs generated from the combined images to those from individual epochs, and from monthly averages, as well as to legacy surveys. They undertook a search for transients, with particular emphasis on excluding false positive sources,but find no confirmed transients, defined here as sources that can be shown to have varied by at least a factor of 10. However, the authors found one source that brightened in a single-epoch image to at least six times the upper limit from the corresponding deep image. They also found a source associated with a z = 0.6 quasar which appears to have brightened by a factor ~3 in one of their deep images, when compared to catalogs from legacy surveys. The authors place new upper limits on the number of transients brighter than 10 mJy: fewer than 0.08 transients deg&lt;sup&gt;-2&lt;/sup&gt; with characteristic timescales of months to years; fewer than 0.02 deg&lt;sup&gt;-2&lt;/sup&gt; with timescales of months; and fewer than 0.009 deg&lt;sup&gt;-2&lt;/sup&gt; with timescales of days. In this study, the authors accepted only as real sources those that are independently detected in both frequencies in at least one epoch (with a position matching tolerance of 50&quot;, corresponding to a false match probability of &lt;2%). Their threshold of ~ 4.2 sigma for detection in a single image corresponds to a threshold of ~ 5.9 sigma in the dual-image catalog. They generated catalogs for the deep fields, consisting only of sources detected at both frequencies, and these are contained in the present HEASARC table. Notice that the authors previously published a list of 425 radio sources in the NDWFS field in the constellation of Bootes in an earlier paper (Bower et al 2010, ApJ, 725, 1792, available as the HEASARC database table PIGSSBOOFD). In the 2013 paper, they have performed a partial re-analysis of these data to conform with the updated analysis techniques used on the other three fields. This table was created by the HEASARC in March 2013 based on electronic versions of Tables 2, 3, 4 and 5 (source lists for each of the 4 fields, ELAIS N1, Lockman, Coma, and NDWFS, respectively) from the reference paper which were obtained from the ApJ web site. The HEASARC has created a new parameter called field_name which identifies in which table/field the source can be found. Thus, to select only sources in the Lockman Hole field, the user should select field_name= &#39;Lockman&#39;. This is a service provided by NASA HEASARC .
820. Allen Telescope Array Twenty-cm Survey (ATATS) Source Catalog
ID:
ivo://nasa.heasarc/atats
Title:
Allen Telescope Array Twenty-cm Survey (ATATS) Source Catalog
Short Name:
ATATS
Date:
28 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains the source catalog from the Allen Telescope Array Twenty-centimeter Survey (ATATS), a multi-epoch (12 visits), 690 deg&lt;sup&gt;2&lt;/sup&gt; radio image and catalog at 1.4 GHz. The survey is designed to detect rare, very bright transients as well as to verify the capabilities of the ATA to form large mosaics. The combined image using data from all 12 ATATS epochs has an rms noise sigma = 3.94 mJy beam&lt;sup&gt;-1&lt;/sup&gt; and a dynamic range of 180, with a circular beam of 150 arcseconds FWHM. It contains 4408 sources to a limiting sensitivity of 5 sigma = 20 mJy beam&lt;sup&gt;-1&lt;/sup&gt;. The authors compare the catalog generated from this 12-epoch combined image to the NRAO VLA Sky Survey (NVSS), a legacy survey at the same frequency, and find that they can measure source positions to better than ~ 20 arcseconds. For sources above the ATATS completeness limit, the median flux density is 97% of the median value for matched NVSS sources, indicative of an accurate overall flux calibration. The authors examine the effects of source confusion due to the effects of differing resolution between the ATATS and NVSS on their ability to compare flux densities. They detect no transients at flux densities greater than 40 mJy in comparison with NVSS and place a 2 sigma upper limit of 0.004 deg&lt;sup&gt;-2&lt;/sup&gt; on the transient rate for such sources. These results suggest that the &gt;~ 1 Jy transients reported by Matsumara et al. (2009, AJ, 138, 787) may not be true transients, but rather variable sources at their flux density threshold. This table was created by the HEASARC in September 2010 based on the electronic version of Table 2 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .

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