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551. A dust model for bet Pic from 0.58 to 870um
ID:
ivo://CDS.VizieR/J/ApJ/823/108
Title:
A dust model for bet Pic from 0.58 to 870um
Short Name:
J/ApJ/823/108
Date:
21 Oct 2021
Publisher:
CDS
Description:
We investigate whether varying the dust composition (described by the optical constants) can solve a persistent problem in debris disk modeling --the inability to fit the thermal emission without overpredicting the scattered light. We model five images of the {beta} Pictoris disk: two in scattered light from the Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph at 0.58{mu}m and HST/Wide Field Camera 3 (WFC3) at 1.16{mu}m, and three in thermal emission from Spitzer/Multiband Imaging Photometer for Spitzer (MIPS) at 24{mu}m, Herschel/PACS at 70{mu}m, and Atacama Large Millimeter/submillimeter Array at 870{mu}m. The WFC3 and MIPS data are published here for the first time. We focus our modeling on the outer part of this disk, consisting of a parent body ring and a halo of small grains. First, we confirm that a model using astronomical silicates cannot simultaneously fit the thermal and scattered light data. Next, we use a simple generic function for the optical constants to show that varying the dust composition can improve the fit substantially. Finally, we model the dust as a mixture of the most plausible debris constituents: astronomical silicates, water ice, organic refractory material, and vacuum. We achieve a good fit to all data sets with grains composed predominantly of silicates and organics, while ice and vacuum are, at most, present in small amounts. This composition is similar to one derived from previous work on the HR 4796A disk. Our model also fits the thermal spectral energy distribution, scattered light colors, and high-resolution mid-IR data from T-ReCS for this disk. Additionally, we show that sub-blowout grains are a necessary component of the halo.
552. Advanced Camera for Surveys
ID:
ivo://archive.stsci.edu/hst/acs
Title:
Advanced Camera for Surveys
Short Name:
HST.ACS
Date:
23 Jul 2020 19:47:47
Publisher:
Space Telescope Science Institute Archive
Description:
HST Advanced Camera for Surveys (ACS) - Images: CCD images between 3,700 - 11
553. Advanced Usage of HiPS and MOCs
ID:
ivo://edu.euro-vo.org/extern/hipsmoc
Title:
Advanced Usage of HiPS and MOCs
Date:
15 Aug 2024 15:17:02
Publisher:
The GAVO DC team
Description:
This course introduces advanced usage of Hierarchical Progressive Surveys (HiPS) and Multi-Order Coverage (MOC) maps in Aladin. Using this document, you will learn how to handle a problem like : “I have a set of images. I would like to select regions in my observations that are above a given threshold in another survey (e.g. at low extinction), retrieve objects from very large catalogs (e.g. Gaia + WISE) in these non-trivial shapes and not-necessarily-connected regions, and combine them to visualise some quantities (e.g. color color diagram).“
554. A 3D view of the Hyades population
ID:
ivo://CDS.VizieR/J/A+A/623/A35
Title:
A 3D view of the Hyades population
Short Name:
J/A+A/623/A35
Date:
21 Oct 2021
Publisher:
CDS
Description:
Our scientific goal is to provide a 3D map of the nearest open cluster to the Sun, the Hyades, combining the recent release of Gaia astrometric data, ground-based parallaxes of sub-stellar member candidates and photometric data from surveys which cover large areas of the cluster. We combined the second Gaia release with ground-based H-band parallaxes obtained with the infrared camera on the 2-m robotic Liverpool telescope to astrometrically identify stellar and sub-stellar members of the Hyades, the nearest open cluster to the Sun. We find 1764 objects within 70 degree radius from the cluster center from the Gaia second data release, whose kinematic properties are consistent with the Hyades. We limit our study to 30pc from the cluster center (47.03+/-0.20pc) where we identify 710 candidate members, including 85 and 385 in the core and tidal radius, respectively. We determine proper motions and parallaxes of eight candidate brown dwarf members and confirm their membership. Using the 3D positions and a model-based mass-luminosity relation we derive a luminosity and mass function in the 0.04 to 2.5M_{sun}_ range. We confirm evidence for mass segregation in the Hyades and find a dearth of brown dwarfs in the core of the cluster. From the white dwarf members we estimate an age of 640^+67^_-49_Myr. We identify a list of members in the Hyades cluster from the most massive stars down to the brown dwarfs. We produce for the first time a 3D map of the Hyades cluster in the stellar and sub-stellar regimes and make available the list of candidate members.
555. A 3D Voronoi+Gapper galaxy cluster finder. II.
ID:
ivo://CDS.VizieR/J/ApJ/869/145
Title:
A 3D Voronoi+Gapper galaxy cluster finder. II.
Short Name:
J/ApJ/869/145
Date:
21 Oct 2021
Publisher:
CDS
Description:
We identify 1901 galaxy clusters (N_g_>=2) with the gapping-filtering in radial velocity (VoML+G) algorithm (Paper I; Campusano+ 2017ApJ...838..109P) on the two-Degree Field Galaxy Redshift Survey (2dFGRS). We present the 341 clusters with at least 10 galaxies that are within 0.009<z<0.14 (the Catalog), of which 254 (~75%) have counterparts in the literature (NED), with the remainder (87) plausibly "new" because of incompleteness of previous searches or unusual galaxy contents. The 207 clusters within z=0.04--0.09 are used to study the properties of the galaxy systems in the nearby universe, including their galaxy contents parameterized by the late-type galaxy fractions (f_L_). For this nearly complete cluster subsample, we find the following: (i) 63% are dominated by early-type galaxies (i.e., the late-type-poor clusters, f_L_<0.5) with corresponding mean multiplicity and logarithmic virial mass (in units of M_{sun}_) of 22+/-1 and 12.91+/-0.04, respectively; and (ii) 37% are dominated by late-type galaxies (i.e., the late-type-rich clusters, f_L_>=0.5) with corresponding mean multiplicity and logarithmic virial mass (in units of M_{sun}_) of 15.7+/-0.9 and 12.66+/-0.07, respectively. The statistical analysis of the late-type fraction distribution supports, with a 3{sigma} confidence level, the presence of two population components. It is suggested that the late-type-poor galaxy systems reflect and extend the class of Abell-APM-EDCC clusters and that the late-type-rich systems (~one-third of the total) belong to a new, previously unappreciated class. The late-type-rich clusters, on average high mass-to-light ratio systems, appear to be more clustered on large scales than the late-type-poor clusters. A class of late-type-rich clusters is not predicted by current theory.
556. AE Aur and iota Ori runaway stars RV curves
ID:
ivo://CDS.VizieR/J/AN/341/645
Title:
AE Aur and iota Ori runaway stars RV curves
Short Name:
J/AN/341/645
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the results of our spectroscopic monitoring observations of the late O-type runaway stars AE Aur and iota Ori, carried out between September 2016 and May 2018 using the Echelle spectrograph FLECHAS at the University Observatory Jena. For both stars, we obtained current radial velocity (RV) measurements with better precision than before. These results can be used for further advanced calculations of their space motion, needed to determine, for example, their place of origin in our Galaxy. In this paper, we describe the observations and the data reduction, as well as the analysis of all spectral data. We find a stable RV for AE Aur and confirm iota Ori as a double-lined spectroscopic binary and derive its current Keplerian orbital elements.
557. Ae/Be stars of Magellanic Bridge in JHKs
ID:
ivo://CDS.VizieR/J/ApJ/658/358
Title:
Ae/Be stars of Magellanic Bridge in JHKs
Short Name:
J/ApJ/658/358
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have found Herbig Ae/Be star candidates in the western region of the Magellanic Bridge. Using the near-infrared camera SIRIUS and the 1.4m telescope IRSF, we surveyed ~3.0{deg}x1.3{deg} (24{deg}<~RA<~36{deg}, -75.0{deg}<~DE<~-73.7{deg}) in the J, H, and Ks bands. On the basis of colors and magnitudes, about 200 Herbig Ae/Be star candidates are selected. Considering the contaminations by miscellaneous sources, such as foreground stars and early-type dwarfs in the Magellanic Bridge, we estimate that about 80 (#40%) of the candidates are likely to be Herbig Ae/Be stars. We also found one concentration of the candidates at the young star cluster NGC 796, strongly suggesting the existence of pre-main-sequence (PMS) stars in the Magellanic Bridge. This is the first detection of PMS star candidates in the Magellanic Bridge, and if they are genuine PMS stars, this could be direct evidence of recent star formation. However, the estimate of the number of Herbig Ae/Be stars depends on the fraction of classical Be stars, and thus a more precise determination of the Be star fraction or observations to differentiate between the Herbig Ae/Be stars and classical Be stars are required.
558. AEGIS: demographics of X-ray and optical AGN
ID:
ivo://CDS.VizieR/J/ApJ/728/38
Title:
AEGIS: demographics of X-ray and optical AGN
Short Name:
J/ApJ/728/38
Date:
21 Oct 2021
Publisher:
CDS
Description:
We develop a new diagnostic method to classify galaxies into active galactic nucleus (AGN) hosts, star-forming galaxies, and absorption-dominated galaxies by combining the [OIII]/H{beta} ratio with rest-frame U-B color. This can be used to robustly select AGNs in galaxy samples at intermediate redshifts (z<1). We compare the result of this optical AGN selection with X-ray selection using a sample of 3150 galaxies with 0.3<z<0.8 and I_AB_<22, selected from the DEEP2 Galaxy Redshift Survey and the All-wavelength Extended Groth Strip International Survey. Among the 146 X-ray sources in this sample, 58% are classified optically as emission-line AGNs, the rest as star-forming galaxies or absorption-dominated galaxies. The latter are also known as "X-ray bright, optically normal galaxies" (XBONGs).
559. AEGIS-X: Chandra deep survey
ID:
ivo://CDS.VizieR/J/ApJS/180/102
Title:
AEGIS-X: Chandra deep survey
Short Name:
J/ApJS/180/102
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the EGIS-X survey, a series of deep Chandra ACIS-I observations of the Extended Groth Strip. The survey comprises pointings at eight separate positions, each with nominal exposure of 200ks, covering a total area of approximately 0.67deg^2^ in a strip of length 2 degrees. We describe in detail an updated version of our data reduction and point-source-detection algorithms used to analyze these data. A total of 1325 band-merged sources have been found to a Poisson probability limit of 4x10^-6^, with limiting fluxes of 5.3x10^-21^W/m2 in the soft (0.5-2keV) band and 3.8x10^-19^W/m2 in the hard (2-10keV) band. We present simulations verifying the validity of our source-detection procedure and showing a very small, <1.5%, contamination rate from spurious sources. Optical/NIR counterparts have been identified from the DEEP2, CFHTLS, and Spitzer/Infrared Array Camera (IRAC) surveys of the same region. Using a likelihood ratio method, we find optical counterparts for 76% of our sources, complete to R_AB_=24.1, and, of the 66% of the sources that have IRAC coverage, 94% have a counterpart to a limit of 0.9uJy at 3.6um (m_AB_=23.8). After accounting for (small) positional offsets in the eight Chandra fields, the astrometric accuracy of Chandra positions is found to be 0"8rms; however, this number depends both on the off-axis angle and the number of detected counts for a given source. All data products described in this paper are made available via a public Web site.
560. AEGIS-X Chandra Extended Groth Strip X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/aegisx
Title:
AEGIS-X Chandra Extended Groth Strip X-Ray Point Source Catalog
Short Name:
AEGISX
Date:
08 Nov 2024
Publisher:
NASA/GSFC HEASARC
Description:
This table contains the X-ray sources detected in the AEGIS-X survey, a series of deep Chandra ACIS-I observations of the Extended Groth Strip (EGS). The survey comprises pointings at eight separate positions, each with nominal exposure of 200 ks, covering a total area of approximately 0.67 deg&lt;sup&gt;2&lt;/sup&gt; in a strip of length 2 degrees. In their paper, the authors describe in detail an updated version of the data reduction and point-source-detection algorithms used to analyze these data. A total of 1325 band-merged sources have been found to a Poisson probability limit of 4 x 10&lt;sup&gt;-6&lt;/sup&gt;, with limiting fluxes of 5.3 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; in the soft (0.5 - 2 keV) band and 3.8 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; in the hard (2 - 10 keV) band. They present simulations verifying the validity of their source-detection procedure and showing a very small, &lt;1.5%, contamination rate from spurious sources. Optical/NIR counterparts have been identified from the DEEP2, CFHTLS, and Spitzer/Infrared Array Camera (IRAC) surveys of the same region. Using a likelihood ratio method, they find optical counterparts for 76% of their sources, complete to R&lt;sub&gt;AB&lt;/sub&gt; = 24.1, and, of the 66% of the sources that have IRAC coverage, 94% have a counterpart to a limit of 0.9 uJy at 3.6 um (m&lt;sub&gt;AB&lt;/sub&gt; = 23.8). After accounting for (small) positional offsets in the eight Chandra fields, the astrometric accuracy of Chandra positions is found to be 0.8 arcseconds rms; however, this number depends both on the off-axis angle and the number of detected counts for a given source. This table was created by the HEASARC in February 2009 based on the electronic versions of Tables 9, 10 and 11 from the paper which were obtained from the Astrophysical Journal web site. It is also available from the CDS at &lt;a href="https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/180/102"&gt;https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/180/102&lt;/a&gt;. This is a service provided by NASA HEASARC .

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