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521. ELM Survey South. I. RVs for 6 new ELM WDs
ID:
ivo://CDS.VizieR/J/ApJ/894/53
Title:
ELM Survey South. I. RVs for 6 new ELM WDs
Short Name:
J/ApJ/894/53
Date:
22 Oct 2021 08:25:16
Publisher:
CDS
Description:
We begin the search for extremely low mass (M<=0.3M_{sun}_, ELM) white dwarfs (WDs) in the southern sky based on photometry from the VST ATLAS and SkyMapper surveys. We use a similar color selection method as the Hypervelocity star survey. We switched to an astrometric selection once Gaia Data Release 2 became available. We use the previously known sample of ELM white dwarfs to demonstrate that these objects occupy a unique parameter space in parallax and magnitude. We use the SOAR 4.1m telescope to test the Gaia-based selection, and identify more than two dozen low mass white dwarfs, including six new ELM white dwarf binaries with periods as short as 2h. The better efficiency of the Gaia-based selection enables us to extend the ELM Survey footprint to the southern sky. We confirm one of our candidates, J0500-0930, to be the brightest (G=12.6mag) and closest (d=72pc) ELM white dwarf binary currently known. Remarkably, the Transiting Exoplanet Survey Satellite (TESS) full-frame imaging data on this system reveals low-level (<0.1%) but significant variability at the orbital period of this system (P=9.5hr), likely from the relativistic beaming effect. TESS data on another system, J0642-5605, reveals ellipsoidal variations due to a tidally distorted ELM WD. These demonstrate the power of TESS full-frame images in confirming the orbital periods of relatively bright compact object binaries.
522. ELQS in SDSS. III. The full ELQS quasar catalog
ID:
ivo://CDS.VizieR/J/ApJ/871/258
Title:
ELQS in SDSS. III. The full ELQS quasar catalog
Short Name:
J/ApJ/871/258
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have designed the Extremely Luminous Quasar Survey (ELQS) to provide a highly complete census of unobscured UV-bright quasars during the cosmic noon, z=2.8-5.0. Here we report the discovery of 70 new quasars in the ELQS South Galactic Cap (ELQS-S) quasar sample, doubling the number of known extremely luminous quasars in 4237.3deg^2^ of the Sloan Digital Sky Survey footprint. These observations conclude the ELQS and we present the properties of the full ELQS quasar catalog, containing 407 quasars over 11838.5deg^2^. Our novel ELQS quasar selection strategy resulted in unprecedented completeness at the bright end and allowed us to discover 109 new quasars in total. This marks an increase of ~36% (109/298) in the known population at these redshifts and magnitudes, while we further are able to retain a selection efficiency of ~80%. On the basis of 166 quasars from the full ELQS quasar catalog, which adhere to the uniform criteria of the Two Micron All Sky Survey point source catalog, we measure the bright-end quasar luminosity function (QLF) and extend it one magnitude brighter than previous studies. Assuming a single power law with exponential density evolution for the functional form of the QLF, we retrieve the best-fit parameters from a maximum likelihood analysis. We find a steep bright-end slope of {beta}~-4.1, and we can constrain the bright-end slope to {beta}<=-3.4 with 99% confidence. The density is well modeled by the exponential redshift evolution, resulting in a moderate decrease with redshift ({gamma}~-0.4).
523. Emission-line galaxies from HETDEX pilot survey
ID:
ivo://CDS.VizieR/J/ApJS/192/5
Title:
Emission-line galaxies from HETDEX pilot survey
Short Name:
J/ApJS/192/5
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a catalog of emission-line galaxies selected solely by their emission-line fluxes using a wide-field integral field spectrograph. This work is partially motivated as a pilot survey for the upcoming Hobby-Eberly Telescope Dark Energy Experiment. We describe the observations, reductions, detections, redshift classifications, line fluxes, and counterpart information for 397 emission-line galaxies detected over 169arcmin^2^ with a 3500-5800{AA} bandpass under 5{AA} full-width-half-maximum (FWHM) spectral resolution. The survey's best sensitivity for unresolved objects under photometric conditions is between 4 and 20x10^-17^erg/s/cm^2^ depending on the wavelength, and Ly{alpha} luminosities between 3x10^42^ and 6x10^42^erg/s are detectable. This survey method complements narrowband and color-selection techniques in the search of high-redshift galaxies with its different selection properties and large volume probed. The four survey fields within the COSMOS, GOODS-N, MUNICS, and XMM-LSS areas are rich with existing, complementary data. We find 105 galaxies via their high-redshift Ly{alpha} emission at 1.9<z<3.8, and the majority of the remainder objects are low-redshift [OII]3727 emitters at z<0.56. The classification between low- and high-redshift objects depends on rest-frame equivalent width (EW), as well as other indicators, where available. Based on matches to X-ray catalogs, the active galactic nuclei fraction among the Ly{alpha} emitters is 6%. We also analyze the survey's completeness and contamination properties through simulations. We find five high-z, highly significant, resolved objects with FWHM sizes >44arcmin^2^ which appear to be extended Ly{alpha} nebulae. We also find three high-z objects with rest-frame Ly{alpha} EW above the level believed to be achievable with normal star formation, EW0>240{AA}.
524. Emission-line stars in Vela Molecular Ridge
ID:
ivo://CDS.VizieR/J/A+AS/104/233
Title:
Emission-line stars in Vela Molecular Ridge
Short Name:
J/A+AS/104/233
Date:
21 Oct 2021
Publisher:
CDS
Description:
(no description available)
525. Empirical relations for cluster RR Lyrae
ID:
ivo://CDS.VizieR/J/A+A/371/579
Title:
Empirical relations for cluster RR Lyrae
Short Name:
J/A+A/371/579
Date:
21 Oct 2021
Publisher:
CDS
Description:
Our former study on the empirical relations between the Fourier parameters of the light curves of the fundamental mode RR Lyrae stars and their basic stellar parameters has been extended to considerably larger data sets. The most significant contribution to the absolute magnitude M_V_ comes from the period P and from the first Fourier amplitude A_1_, but there are statistically significant contributions also from additional higher order components, most importantly from A_3_ and in a lesser degree from the Fourier phase phi_51_. When different colors are combined in reddening-free quantities, we obtain basically period-luminosity-color relations. From the standard deviations of the various regressions, an upper limit can be obtained on the overall inhomogeneity of the reddening in the individual clusters. This yields {sigma}_E(B-V)_<0.012mag, which also implies an average minimum observational error of {sigma}_V_>0.018mag.
526. End of red sequence galaxies in Galaxy Zoo
ID:
ivo://CDS.VizieR/J/MNRAS/420/1684
Title:
End of red sequence galaxies in Galaxy Zoo
Short Name:
J/MNRAS/420/1684
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a study of local post-starburst galaxies (PSGs) using the photometric and spectroscopic observations from the Sloan Digital Sky Survey and the results from the Galaxy Zoo project. We find that the majority of our local PSG population have neither early- nor late-type morphologies but occupy a well-defined space within the colour-stellar mass diagram, most notably, the low-mass end of the 'green valley' below the transition mass thought to be the mass division between low-mass star-forming galaxies and high-mass passively evolving bulge-dominated galaxies.
527. Energetic Gamma-Ray Event Telescope: 10 channel data
ID:
ivo://nasa.heasarc/skyview/egret3d
Title:
Energetic Gamma-Ray Event Telescope: 10 channel data
Short Name:
EGRET3D
Date:
25 Apr 2025
Publisher:
NASA/GSFC HEASARC
Description:
These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-10000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels. <P> The EGRET 3D map is comprised of ten channels with the following energy ranges: <UL> <LI>Channel 1 30-50 MeV <LI>Channel 2 50-70 MeV <LI>Channel 3 70-100 MeV <LI>Channel 4 100-150 MeV <LI>Channel 5 150-300 MeV <LI>Channel 6 300-500 MeV <LI>Channel 7 500-1000 MeV <LI>Channel 8 1000-2000 MeV <LI>Channel 9 2000-4000 MeV <LI>Channel 10 4000-10000 MeV </ul> <p> The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
528. Energetic Gamma-Ray Event Telescope: Hard
ID:
ivo://nasa.heasarc/skyview/egret
Title:
Energetic Gamma-Ray Event Telescope: Hard
Short Name:
EGRET
Date:
25 Apr 2025
Publisher:
NASA/GSFC HEASARC
Description:
These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-100000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels. <P> The EGRET 3D map is comprised of ten channels with the following energy ranges: <UL> <LI>Channel 1 30-50 MeV <LI>Channel 2 50-70 MeV <LI>Channel 3 70-100 MeV <LI>Channel 4 100-150 MeV <LI>Channel 5 150-300 MeV <LI>Channel 6 300-500 MeV <LI>Channel 7 500-1000 MeV <LI>Channel 8 1000-2000 MeV <LI>Channel 9 2000-4000 MeV <LI>Channel 10 4000-10000 MeV </ul> <p> The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
529. Enhanced 3XMM catalogue (3XMMe)
ID:
ivo://CDS.VizieR/IX/47
Title:
Enhanced 3XMM catalogue (3XMMe)
Short Name:
IX/47
Date:
21 Oct 2021
Publisher:
CDS
Description:
The enhanced 3XMM catalogue (designated 3XMMe) is one of the core elements of the Arches project, representing the X-ray source basis for the cross-correlations with other multi-wavelength catalogues. The 3XMMe catalogue is a derivative of the latest increment of the 3XMM catalogue, i.e. 3XMM-DR5, that was publicly released in April 2015 (Rosen et al., 2016A&A...590A...1R, Cat. XI/46)), tailored for the purposes of the Arches project. The 3XMM-DR5 catalogue, available from the XMM-Newton Science Archive (http://xmm.esac.esa.int/xsa/), the XMM-Newton Survey Science Centre (SSC) (http://xmmssc.irap.omp.eu) and other sites listed on the SSC site, contains 565962 detections arising from 396910 unique sources drawn from 7781 XMM observations. These numbers include detections from 356 sub-pointings made in mosaic mode. Arches wed site : http://www.arches-fp7.eu .
530. Environmental dependence of SN Ia luminosities
ID:
ivo://CDS.VizieR/J/ApJ/854/24
Title:
Environmental dependence of SN Ia luminosities
Short Name:
J/ApJ/854/24
Date:
21 Oct 2021
Publisher:
CDS
Description:
It is established that there is a dependence of the luminosity of type Ia supernovae (SNe Ia) on environment: SNe Ia in young, star-forming, metal-poor stellar populations appear fainter after light-curve shape corrections than those in older, passive, metal-rich environments. This is accounted for in cosmological studies using a global property of the SN host galaxy, typically the host galaxy stellar mass. However, recent low-redshift studies suggest that this effect manifests itself most strongly when using the local star formation rate (SFR) at the SN location, rather than the global SFR or the stellar mass of the host galaxy. At high-redshift, such local SFRs are difficult to determine; here, we show that an equivalent local correction can be made by restricting the SN Ia sample in globally star-forming host galaxies to a low-mass host galaxy subset (<=10^10^M_{sun}_). Comparing this sample of SNe Ia (in locally star-forming environments) to those in locally passive host galaxies, we find that SNe Ia in locally star-forming environments are 0.081+/0.018 mag fainter (4.5{sigma}), consistent with the result reported by Rigault+ (2013A&A...560A..66R), but our conclusion is based on a sample ~5 times larger over a wider redshift range. This is a larger difference than when splitting the SN Ia sample based on global host galaxy SFR or host galaxy stellar mass. This method can be used in ongoing and future high-redshift SN surveys, where local SN Ia environments are difficult to determine.

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