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2521. CFHT M33 extended sources catalog
ID:
ivo://CDS.VizieR/J/ApJ/720/1674
Title:
CFHT M33 extended sources catalog
Short Name:
J/ApJ/720/1674
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a catalog of 2990 extended sources in a 1x1{deg} area centered on M33 using the MegaCam camera on the 3.6m Canada-France-Hawaii Telescope. The catalog includes 599 new candidate stellar clusters, 204 previously confirmed clusters, 1969 likely background galaxies, and 218 unknown extended objects. We present ugriz integrated magnitudes of the candidates and confirmed star clusters (SCs) as well as the full width at half maximum, ellipticity, and stellarity. Based on the properties of the confirmed SCs, we select a sub-sample of highly probable clusters composed of 246 objects. The integrated photometry of the complete cluster catalog reveals a wide range of colors of -0.4<(g-r)<1.5 and -1.0<(r-i)<1.0 with no obvious cluster subpopulations. Comparisons with models of simple stellar populations suggest a large range of ages some as old as ~10Gyr.
2522. CFHT r- and z-band images 28 Planck sources
ID:
ivo://CDS.VizieR/J/A+A/587/A23
Title:
CFHT r- and z-band images 28 Planck sources
Short Name:
J/A+A/587/A23
Date:
21 Oct 2021
Publisher:
CDS
Description:
The Planck catalogue of SZ sources limits itself to a significance threshold of 4.5 to ensure a low contamination rate by false cluster candidates. This means that only the most massive clusters at redshift z>0.5, and in particular z>0.7, are expected to enter into the catalogue, with a large number of systems in that redshift regime being expected around and just below that threshold. In this paper, we follow-up a sample of SZ sources from the Planck SZ catalogues from 2013 and 2015. In the latter maps, we consider detections around and at lower significance than the threshold adopted by the Planck Collaboration. To keep the contamination rate low, our 28 candidates are chosen to have significant WISE detections, in combination with non-detections in SDSS/DSS, which effectively selects galaxy cluster candidates at redshifts z>~0.5. By taking r- and z-band imaging with MegaCam@CFHT, we bridge the 4000{AA} rest-frame break over a significant redshift range, thus allowing accurate redshift estimates of red-sequence cluster galaxies up to z~0.8. After discussing the possibility that an overdensity of galaxies coincides -by chance- with a Planck SZ detection, we confirm that 16 of the candidates have likely optical counterparts to their SZ signals, 13 (6) of which have an estimated redshift z>0.5 (z>0.7). The richnesses of these systems are generally lower than expected given the halo masses estimated from the Planck maps. However, when we follow a simplistic model to correct for Eddington bias in the SZ halo mass proxy, the richnesses are consistent with a reference mass-richness relation established for clusters detected at higher significance. This illustrates the benefit of an optical follow-up, not only to obtain redshift estimates, but also to provide an independent mass proxy that is not based on the same data the clusters are detected with, and thus not subject to Eddington bias
2523. CFHT ugi photometry of globular clusters in M85
ID:
ivo://CDS.VizieR/J/ApJ/872/202
Title:
CFHT ugi photometry of globular clusters in M85
Short Name:
J/ApJ/872/202
Date:
21 Oct 2021
Publisher:
CDS
Description:
We survey globular clusters (GCs) in M85 using ugi-band images of a 1{deg}x1{deg} field obtained with the MegaCam at the 3.6m Canada-France-Hawaii Telescope. We identify 1318 GC candidates with 20.0mag<g_0_<23.5mag in the entire survey region. Their radial number density profile is well fit by a Sersic profile with n=2.58_-0.33_^+0.43^ and effective radius R_e,GCS_=4.14' (=22kpc), showing that the candidates at R<20' are mostly genuine GCs in M85. We estimate the total number of GCs, N(total)=1216_-50_^+82^, and the specific frequency, S_N_=1.41_-0.06_^+0.10^. The overall color distribution of the GCs in M85 is bimodal, but the GCs in the central region at R<2' do not show a bimodal distribution clearly. The radial number density profile and surface number density map of the blue GCs (BGCs) show more extended structures than those of the red GCs (RGCs). The spatial distributions of both BGCs and RGCs are elongated, similar to that of the galaxy stellar light. The number fraction of the RGCs in the central region is much smaller compared to those in other early-type galaxies of similar luminosity. The mean (g-i)_0_ color of the RGCs in M85 is about 0.1mag bluer than typical values for other Virgo early-type galaxies of similar luminosity, indicating that a significant fraction of the RGCs in M85 may be younger than typical GCs. These results indicate that M85 might have undergone a major wet merger recently.
2524. 4C 23.56 field deep imaging
ID:
ivo://CDS.VizieR/J/ApJS/109/367
Title:
4C 23.56 field deep imaging
Short Name:
J/ApJS/109/367
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'>4mag in the field, including two with I-K'>6mag.
2525. C/2012 F6 (Lemmon) and C/2012 S1 (ISON) maps
ID:
ivo://CDS.VizieR/J/ApJ/792/L2
Title:
C/2012 F6 (Lemmon) and C/2012 S1 (ISON) maps
Short Name:
J/ApJ/792/L2
Date:
21 Oct 2021
Publisher:
CDS
Description:
Results are presented from the first cometary observations using the Atacama Large Millimeter/Submillimeter Array (ALMA), including measurements of the spatially resolved distributions of HCN, HNC, H_2_CO, and dust within the comae of two comets: C/2012 F6 (Lemmon) and C/2012 S1 (ISON), observed at heliocentric distances of 1.5 AU and 0.54 AU, respectively. These observations (with angular resolution ~0.5"), reveal an unprecedented level of detail in the distributions of these fundamental cometary molecules, and demonstrate the power of ALMA for quantitative measurements of the distributions of molecules and dust in the inner comae of typical bright comets. In both comets, HCN is found to originate from (or within a few hundred kilometers of) the nucleus, with a spatial distribution largely consistent with spherically symmetric, uniform outflow. By contrast, the HNC distributions are clumpy and asymmetrical, with peaks at cometocentric radii ~500-1000km, consistent with release of HNC in collimated outflow(s). Compared to HCN, the H_2_ CO distribution in comet Lemmon is very extended. The interferometric visibility amplitudes are consistent with coma production of H_2_CO and HNC from unidentified precursor material(s) in both comets. Adopting a Haser model, the H_2_CO parent scale length is found to be a few thousand kilometers in Lemmon and only a few hundred kilometers in ISON, consistent with the destruction of the precursor by photolysis or thermal degradation at a rate that scales in proportion to the solar radiation flux.
2526. CFRS XI: High-redshift field galaxies morphology
ID:
ivo://CDS.VizieR/J/ApJ/464/79
Title:
CFRS XI: High-redshift field galaxies morphology
Short Name:
J/ApJ/464/79
Date:
21 Oct 2021
Publisher:
CDS
Description:
The 143 galaxies with secure redshifts (Z_median_=0.62) from the 1415+52 field of the Canada-France Redshift Survey have been imaged with median seeing of 0.67" (FWHM). Structural parameters have been derived by fitting multicomponent models and the results confirm two phenomena seen in a smaller sample of galaxies imaged with the Hubble Space Telescope. First, 11+/-3% of the galaxies lie off the normal locus of color versus bulge fraction B/T. This class of objects ("blue nucleated galaxies," or BNGs) was identified using HST observations (Schade et al. 1995ApJ...451L...1S, hereafter CFRS IX), and it was shown that they are associated with peculiar/asymmetric structure and merger/interactions. The observed frequency of BNGs in this sample is 14+/-4% 0.5<z<1.2 and 6^+6^_-3_% at 0.2<z<0.5, but the true frequency is likely to be a factor ~2 higher after corrections are made for the effect of asymmetric/peculiar structures. Galaxy disks at 0.5<z<1.1 are found to have a mean rest-frame, inclination-corrected central surface brightness of {mu}_AB_(B)=19.8+/-0.1mag/arcsec^2^, ~1.6mag brighter than the Freeman (1970ApJ...160..811F) value. At low redshift (0.2<z<0.5) the mean surface brightness [{mu}_AB_(B)=21.3+/-0.25] is consistent with the Freeman value. These results are consistent with the HST observations. With larger numbers of galaxies and therefore more statistical weight they demonstrate the capabilities, and limits, of ground-based work in the study of galaxy morphology at high redshift.
2527. CFRS XIV. Field galaxies up to z=1
ID:
ivo://CDS.VizieR/J/ApJ/481/49
Title:
CFRS XIV. Field galaxies up to z=1
Short Name:
J/ApJ/481/49
Date:
21 Oct 2021
Publisher:
CDS
Description:
The spectral properties of more than 400 Canada-France Redshift Survey (CFRS) galaxies and their changes over the redshift interval 0<=z<=1.3 are investigated. Emission-line intensities and equivalent widths for accessible lines have been measured, as well as continuum color indices based on 200{AA} wide spectral regions.
2528. CG 12 Chandra X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/cg12cxo
Title:
CG 12 Chandra X-Ray Point Source Catalog
Short Name:
CG12CXO
Date:
25 Apr 2025
Publisher:
NASA/GSFC HEASARC
Description:
The mysterious high Galactic latitude cometary globule CG 12 has been observed with the ACIS detector on board the Chandra X-Ray Observatory. 128 X-ray sources are detected, of which half are likely young stars formed within the globule&#39;s head. This new population of &gt;~ 50 T Tauri stars and one new embedded protostar is far larger than the previously reported few intermediate-mass and two protostellar members of the cloud. Most of the newly discovered stars have masses of 0.2-0.7 M&lt;sub&gt;solar&lt;/sub&gt;, and 9% - 15% have K-band excesses from inner protoplanetary disks. X-ray properties provide an independent distance estimate consistent with the unusual location of CG 12 &gt;~200 pc above the Galactic plane. The star formation efficiency in CG 12 appears to be 15% - 35%, far above that seen in other triggered molecular globules. The median photometric age found for the T Tauri population, assuming Siess et al. (2000, A&amp;A, 358, 593) isochrones, is ~4 Myr with a large spread of &lt;1 - 20 Myr and ongoing star formation in the molecular cores. The stellar age and spatial distributions are inconsistent with a simple radiation-driven implosion (RDI) model and suggest either that CG 12 is an atypically large shocked globule or that it has been subject to several distinct episodes of triggering and ablation. In their paper the authors report a previously unnoticed group of B-type stars northwest of CG 12 that may be the remnants of an OB association that produced multiple supernova explosions that could have shocked and ablated the cloud over a 15 - 30 Myr period. HD 120958 (B3e), the most luminous member of the group, may be currently driving an RDI shock into the CG 12 cloud. The current project combines four X-ray observations of the globule: &lt;pre&gt; Field ObsID Start Time Expo. R.A. Decl. Roll Angle (UT) (ks) (J2000.0) (deg) I.... 6423 2006 Apr 15 16:19:17 30.8 13 57 44.52 39 58 48.31 11.5 II... 6424 2006 Jun 02 07:25:09 3.1 13 57 42.87 39 43 01.76 285.0 III.. 6425 2006 Apr 13 08:44:08 3.1 13 56 19.40 39 42 47.94 14.7 IV... 6426 2006 Apr 15 12:54:20 3.1 13 56 19.40 39 58 48.09 11.1 &lt;/pre&gt; where the units of right ascension are hours, minutes, and seconds, and the units of declination are degrees, arcminutes, and arcseconds, ObsID values are from the Chandra Observation Catalog, exposure times are the sum of Good Time Intervals (GTIs) for the CCD at the telescope aim point (CCD3) minus 1.3% to account for CCD readouts, and the aim points and roll angles are obtained from the satellite aspect solution before astrometric correction was applied. There is one primary field (I in Fig. 1 of the reference paper) with ~31 ks exposure directed at the globule&#39;s core and three secondary fields (II, III, and IV in Fig. 1) with ~3 ks exposures positioned contiguously to the north and west of the core. The primary pointing is intended to detect the population of pre-main sequence (PMS) stars forming in the molecular head of the globule. The secondary pointings are designed to locate an older population of stars expected if the present cloud is only the ablated remnant of a larger cloud that experienced sequential star formation triggering events, similar to the sequence of stars found in the authors&#39; Chandra study of IC 1396N (Getman et al. 2007, ApJ, 654, 316, available in Browse as the IC1396NCXO table). Source searching was performed with data images and exposure maps constructed at three spatial resolutions (0.5&quot;, 1.0&quot;, and 1.4&quot; pixel&lt;sup&gt;-1&lt;/sup&gt;) using the CIAO wavdetect tool. The authors ran wavdetect with a low threshold P = 10&lt;sup&gt;-5&lt;/sup&gt;, which is highly sensitive but permits false detections at this point in the analysis. This was followed by visual examination to locate other candidate sources, mainly close doubles and candidate sources near the detection threshold. Using ACIS Extract, photons were extracted within polygonal contours of ~90% encircled energy using position-dependent models of the PSF. The background was measured locally in source-free regions. Due to the very low, spatially invariant ACIS-I background in the Chandra observations of CG 12, there is a one-to-one correspondence between a source&#39;s significance and net counts. Following the procedure of Getman et al. (2007, ApJ, 654, 316), the list of candidate sources ws trimmed to omit sources with fewer than ~5 estimated source net counts, net full-band counts/PSF fraction &lt;~ 4.5. In the case of the CG 12 observations, the above criterion is equivalent to accepting sources with a source significance of &gt;~ 1.1. Thus, most of the statistically insignificant source candidates found during the wavdetect step were eliminated by the application of these source existence criteria. For Chandra sources with &gt; 20 net counts, the authors performed spectral analysis with the XSPEC spectral fitting package version 12.2. The unbinned source and background spectra were fitted with one-temperature APEC plasma emission models using the maximum likelihood method. They assumed 0.3 times solar elemental abundances previously suggested as typical for young stellar objects (YSOs) in other star-forming regions. Solar abundances were taken from Anders &amp; Grevesse (1989, Geochim. Cosmochim. Acta, 53, 197). X-ray absorption was modeled using the atomic cross sections of Morrison &amp; McCammon (1983, ApJ, 270, 119). For absorbed thermal spectra characteristics of PMS stars, the absorption N&lt;sub&gt;H&lt;/sub&gt; can be estimated to roughly a factor of 2 precision for 20 count sources. This table was created by the HEASARC in October 2010 based on the electronic versions of Tables 2, 3 and 4 from the paper which were obtained from the CDS (their catalog J/ApJ/673/331). This is a service provided by NASA HEASARC .
2529. 9C 15-GHz Ryle Telescope Survey of VSA Fields Source Catalog
ID:
ivo://nasa.heasarc/rtv9c15ghz
Title:
9C 15-GHz Ryle Telescope Survey of VSA Fields Source Catalog
Short Name:
RTV9C15GHZ
Date:
25 Apr 2025
Publisher:
NASA/GSFC HEASARC
Description:
The fields chosen for the first observations of the cosmic microwave background (CMB) with the Very Small Array (VSA) have been surveyed with the Ryle Telescope at 15 GHz. The authors have covered three regions around RA = 00&lt;sup&gt;h&lt;/sup&gt;20&lt;sup&gt;m&lt;/sup&gt; and Dec = +30&lt;sup&gt;o&lt;/sup&gt;, RA = 09&lt;sup&gt;h&lt;/sup&gt;40m and Dec = +32&lt;sup&gt;o&lt;/sup&gt; and RA = 15&lt;sup&gt;h&lt;/sup&gt;40&lt;sup&gt;m&lt;/sup&gt; and Dec = +43&lt;sup&gt;o&lt;/sup&gt; (J2000.0), comprising an area of 520 deg&lt;sup&gt;2&lt;/sup&gt;. There are 465 sources in this entire area which are above the estimated completeness limit of ~ 25 mJy, although a total of ~ 760 sources were detected, some as faint as 10 mJy. The prime motivation of this study was to define a catalog of the foreground sources that must be monitored by the VSA during its observations at 34 GHz. In particular, it provides a means of identifying GigaHertz peaked spectrum (GPS) sources, which are important for the study of radio source evolution, as well as being a significant foreground for CMB observations over a range of wavelengths. Since this will be a new and quite extensive survey, it was desgignated as &#39;9C&#39; or the Ninth Cambridge survey. For the purpose of this particular component of the 9C survey, the authors designated as a subset, 3 circular areas, VSA1, VSA2 and VSA3, defined by the properties listed in Table 2 of the reference paper and reproduced below: &lt;pre&gt; Field Centre J2000.0 Center B1950.0 Radius Area RA Dec RA Dec (degrees) (sq. degrees) VSA1 00 17 36.5 +30 16 39 00 15 00.0 +30 00 00 5.5 95.0 VSA2 09 40 57.7 +31 46 21 09 38 00.0 +32 00 00 6.0 113.0 VSA3 15 36 42.7 +43 20 11 15 35 00.0 +43 30 00 5.0 78.5 &lt;/pre&gt; There are 242 sources which were both above the 25 mJy completeness limit and were in the 286.5 deg&lt;sup&gt;2&lt;/sup&gt; contained within these 3 circular fields. These source were listed in 3 tables in the reference paper, Table 4 (VSA1), Table 5 (VSA2) and Table 6 (VSA3). These have been combined into this one HEASARC table, in which the HEASARC added a new parameter vsa_field, which is set to 1 for the VSA1 sources, 2 for the VSA2 sources, and 3 for the VSA3 sources. This table was created in November 2010 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/342/915"&gt;CDS catalog J/MNRAS/342/915&lt;/a&gt; files table4.dat, table5.dat and table6.dat. This is a service provided by NASA HEASARC .
2530. 7C(G) 151-MHz Northern Galactic Plane Survey Catalog
ID:
ivo://nasa.heasarc/gp7c151mhz
Title:
7C(G) 151-MHz Northern Galactic Plane Survey Catalog
Short Name:
GP7C151MHZ
Date:
25 Apr 2025
Publisher:
NASA/GSFC HEASARC
Description:
Results from a survey of the northern Galactic plane (at Declination &gt;= 30&lt;sup&gt;o&lt;/sup&gt; at 151 MHz made with the Cambridge Low Frequency Synthesis Telescope (CLFST) are presented in this table. This survey was designated the 7C(G) - i.e. the Galactic portion of the then-ongoing 7C surveys. The 7C(G) covers the regions 80&lt;sup&gt;o&lt;/sup&gt; &lt; l &lt; 104&lt;sup&gt;o&lt;/sup&gt; and 126&lt;sup&gt;o&lt;/sup&gt; &lt; l &lt; 180&lt;sup&gt;o&lt;/sup&gt;, for |b| &lt;= 5.5&lt;sup&gt;o&lt;/sup&gt;, and has some coverage to |b| ~ 9&lt;sup&gt;o&lt;/sup&gt;, with a resolution of ~70 x70 cosec{delta} arcsec&lt;sup&gt;2&lt;/sup&gt; (RA x Dec). The observations, data reduction and calibration of this survey are described in the reference paper, and the catalog of 6262 compact sources, with a completeness limit of ~ 0.25 Jy (250 mJy) over most of the survey region, is presented in this table. The catalog has an rms positional accuracy of better than 10 arcseconds, and the flux densities are tied to the scale of Roger, Bridle &amp; Costain (1973, AJ, 78, 1030) with an accuracy of better than 10 per cent. This table was created by the HEASARC in October 2010 based on CDS table J/MNRAS/294/607 file 7cg.dat. This is a service provided by NASA HEASARC .

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