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1951. CALSPEC: WFC3 infrared grism spectrophotometry
ID:
ivo://CDS.VizieR/J/AJ/157/229
Title:
CALSPEC: WFC3 infrared grism spectrophotometry
Short Name:
J/AJ/157/229
Date:
21 Oct 2021
Publisher:
CDS
Description:
The collections of spectral energy distributions (SEDs) in the Hubble Space Telescope (HST) CALSPEC database are augmented by 19 infrared (IR) SEDs from Wide Field Camera 3 (WFC3) IR grism spectra. Together, the two IR grisms, G102 and G141, cover the 0.8-1.7 {mu}m range with resolutions of R=200 and 150, respectively. These new WFC3 SEDs overlap existing CALSPEC Space Telescope Imaging Spectrograph (STIS) standard star flux distributions at 0.8-1 {mu}m with agreement to ~<1%. Some CALSPEC standards already have near-IR camera and multi-object spectrogragh (NICMOS) SEDs; but in their overlap region at 0.8-1.7 {mu}m, the WFC3 data have better wavelength accuracy, better spectral resolution, better repeatability, and, consequently, better flux distributions of ~1% accuracy in our CALSPEC absolute flux SEDs versus ~2% for NICMOS. With the improved SEDs in the WFC3 range, the modeled extrapolations to 32 {mu}m for the James Webb Space Telescope flux standards begin to lose precision longward of the 1.7 {mu}m WFC3 limit, instead of at the 1.0-{mu}m-long wavelength limit for STIS. For example, the extrapolated IR flux longward of 1.7 {mu}m for 1808347 increases by ~1% for the model fit to the data with WFC3, instead of just to the STIS SED alone.
1952. Caltech Faint Galaxy Redshift Survey. XIV
ID:
ivo://CDS.VizieR/J/AJ/120/2190
Title:
Caltech Faint Galaxy Redshift Survey. XIV
Short Name:
J/AJ/120/2190
Date:
21 Oct 2021
Publisher:
CDS
Description:
Morphological classifications are reported for Hubble Space Telescope images of 241 galaxies in the Hubble Deep Field and its flanking fields with measured redshifts in the interval 0.25<z<1.2, drawn from a magnitude-limited redshift survey to R=24.0. The galaxies are divided into three groups with redshifts in the intervals 0.25-0.6, 0.6-0.8, and 0.8-1.2. R_606_ images from the first group and I814 images from the second and third groups are compared with B-band images of nearby galaxies. All classifications were therefore made at approximately the same rest wavelength. Selection biases are discussed.
1953. Caltech Faint Galaxy Redshift Survey. XV.
ID:
ivo://CDS.VizieR/J/AJ/122/611
Title:
Caltech Faint Galaxy Redshift Survey. XV.
Short Name:
J/AJ/122/611
Date:
21 Oct 2021
Publisher:
CDS
Description:
To circumvent the spatial effects of resolution on galaxy classification, the images of 233 objects of known redshift in the Hubble Deep Field (HDF) and its flanking fields that have redshifts in the range 0.20<z<1.10 were degraded to the resolution that they would have had if they were all located at a redshift of z=1.00. As in Paper XIV (Cat. <J/AJ/120/2190>) of the present series, the effects of shifts in rest wavelength were mitigated by using R-band images for the classification of galaxies with 0.2<z<0.6 and I-band images for objects with redshifts 0.6<z<1.1. A special effort was made to search for bars in distant galaxies. The present data strongly confirm the previous conclusion that the Hubble tuning fork diagram only provides a satisfactory framework for the classification of galaxies with z<0.3. More distant disk galaxies are often difficult to shoehorn into the Hubble classification scheme. The paucity of barred spirals and grand-design spirals at large redshifts is confirmed. It is concluded that the morphology of disk galaxies observed at look-back times smaller than 3-4Gyr differs systematically from that of more distant galaxies viewed at look-back times of 4-8Gyr. The disks of late-type spirals at z>0.5 are seen to be more chaotic than those of their nearer counterparts. Furthermore, the spiral structure in distant early-type spirals appears to be less well developed than it is in nearby early galaxies.
1954. CALYMHA survey. I.
ID:
ivo://CDS.VizieR/J/MNRAS/466/1242
Title:
CALYMHA survey. I.
Short Name:
J/MNRAS/466/1242
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the CAlibrating LYMan-{alpha} with H{alpha} (CALYMHA) pilot survey and new results on Lyman {alpha} (Ly{alpha}) selected galaxies at z~2. We use a custom-built Ly{alpha} narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z=2.23H{alpha} HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3{sigma} line flux limit of ~4x10^-17^erg/s/cm^2^, and a Ly{alpha} luminosity limit of ~10^42.3^erg/s. We find 188 Ly{alpha} emitters over 7.3x10^5^Mpc^3^, but also find significant numbers of other line-emitting sources corresponding to HeII, CIII] and CIV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Ly{alpha} luminosity function at z=2.23 is very well described by a Schechter function up to L_Ly{alpha}_~=10^43^erg/s^ with L*=10^42.59(10^42.75^-10^42.01^)erg/s, {phi}*=10^-3.09^(10^-3.43^-10^2.95)Mpc^-3^ and {alpha}=-1.75+/-0.25. Above L_Ly{alpha}_~=10^43^erg/s, the Ly{alpha} luminosity function becomes power-law like, driven by X-ray AGN. We find that Ly{alpha}-selected emitters have a high escape fraction of 37+/-7 per cent, anticorrelated with Ly{alpha} luminosity and correlated with Ly{alpha} equivalent width. Ly{alpha} emitters have ubiquitous large (~=40kpc) Ly{alpha} haloes, ~2 times larger than their H{alpha} extents. By directly comparing our Ly{alpha} and H{alpha} luminosity functions, we find that the global/overall escape fraction of Ly{alpha} photons (within a 13kpc radius) from the full population of star-forming galaxies is 5.1+/-0.2 per cent at the peak of the star formation history. An extra 3.3+/-0.3 per cent of Ly{alpha} photons likely still escape, but at larger radii.
1955. Camelopardalis dust and molecular clouds
ID:
ivo://CDS.VizieR/J/BaltA/16/327
Title:
Camelopardalis dust and molecular clouds
Short Name:
J/BaltA/16/327
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using infrared photometric data extracted from the 2MASS, IRAS and MSX databases, 142 suspected young stellar objects (YSOs) are selected from about 2 million stars in the Camelopardalis segment of the Milky Way limited by Galactic coordinates, b=132-158{deg},+/-12{deg}.
1956. Canadian Galactic Plane Survey (CGPS) 1420-MHz Compact Source Catalog
ID:
ivo://nasa.heasarc/cgpsngpcat
Title:
Canadian Galactic Plane Survey (CGPS) 1420-MHz Compact Source Catalog
Short Name:
CGPSNGPCAT
Date:
21 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains a catalog of compact sources of radio emission at 1420 MHz in the northern Galactic plane from the Canadian Galactic Plane Survey (CGPS). The catalog contains 72,758 compact sources with an angular size less than 3 arcminutes within the Galactic longitude range 52 &lt; l&lt;sub&gt;II&lt;/sub&gt; &lt; 192 degrees down to a 5-sigma detection level of ~1.2 mJy. Linear polarization properties are included for 12,368 sources with signals greater than 4 x sigma&lt;sub&gt;QU&lt;/sub&gt; in the CGPS Stokes Q and U images at the position of the total intensity peak. In the reference paper, the authors compare the CGPS flux densities with the catalogued flux densities in the Northern VLA Sky Survey (NVSS) catalog for 10,897 isolated unresolved sources with CGPS flux density greater than 4 mJy in order to search for sources that show variable flux density on timescales of several years. They identify 146 candidate variables that exhibit high fractional variations between the two surveys. In addition, they identify 13 candidate transient sources that have CGPS flux density above 10 mJy but that are not detected in the NVSS. In the CGPS, the Synthesis Telescope at the Dominion Radio Astrophysical Observatory (the DRAO ST) provided arcminute-resolution images of the radio continuum and atomic-hydrogen line emission of the northern Galactic Plane. The CGPS DRAO radio continuum observations provided images of Stokes I, Q, and U in four 7.5-MHz sub-bands spanning 35 MHz, centered on 1420 MHz. The observations were carried out in three phases beginning in 1995 and ending in 2009. The sky coverage of each phase and the observing dates are listed in Table 1 of the reference paper. The Galactic plane was covered with a width in Galactic latitude of 9 degrees, centered at b&lt;sub&gt;II&lt;/sub&gt; = 1 degree to accommodate the warp of the Galactic disk. The longitude coverage was constrained by the southern Declination limit of ~20 degrees, the range that could be effectively imaged by a linear east-west synthesis telescope array. The Phase II observations included an extension to higher latitudes (b&lt;sub&gt;II&lt;/sub&gt; = 17.5 degrees) over a restricted range of longitude. In this table, we present the CGPS 1420-MHz compact source catalog covering 1,464 square degrees and spanning a range of 140 degrees of Galactic longitude between 52 and 192 degrees. This table was created by the HEASARC in June 2017 based upon a machine-readable version of Table 2 from the reference paper that was obtained from the AJ web site. This is a service provided by NASA HEASARC .
1957. CANARY ELT-elongated LGS AO telemetry
ID:
ivo://CDS.VizieR/J/A+A/649/A158
Title:
CANARY ELT-elongated LGS AO telemetry
Short Name:
J/A+A/649/A158
Date:
22 Feb 2022
Publisher:
CDS
Description:
Laser Guide Stars (LGS) allow Adaptive Optics (AO) systems to reach higher sky coverage and correct the atmospheric turbulence on wider field of views. However LGS suffer from limitations, among which is their apparent elongation which can reach 20 arcseconds when observed with large aperture telescopes such as the European Southern Observatory's 39m telescope. The consequences of these extreme elongations have been studied in simulations and lab experiments, but never on-sky. Yet understanding and mitigating those effects is key to taking full advantage of the Extremely Large Telescope (ELT) six LGS. In this paper, we study the impact of wavefront sensing with an ELT-scale elongated LGS using data obtained on-sky with the AO demonstrator CANARY on the William Herschel telescope (WHT) and ESO's Wendelstein LGS unit. CANARY observed simultaneously a natural guide star and a superimposed LGS launched from a telescope placed 40 m away from the WHT pupil. Comparison of the wavefronts measured with each guide star allows to build an error breakdown of the elongated LGS wavefront sensing. With this error breakdown, we isolate the contribution of the LGS elongation and study its impact. We also investigate the effects of truncating or undersampling the LGS spots. We successfully used the elongated LGS wavefront sensor (WFS) to drive the AO loop during on-sky operations, but it necessitated regular calibrations of the non-common path aberrations on the LGS WFS arm. In the off-line processing of the data collected on-sky, we separate the error term encapsulating the impact of LGS elongation in a dynamic and quasi-static component. We measure errors varying from 0 to 160nm rms for the dynamic error and are able to link it with turbulence strength and spot elongation. The quasi-static errors are significant and vary between 20 to 200nm rms depending on the conditions. They also increase by as much as 70nm in the course of 10 min. We do not observe any impact when undersampling the spots with pixel scales as large as 1.95 arcseconds but significant errors appear when truncating the spots. These errors appear for field of views smaller than 10.4 to 15.6 arcseconds, depending on the spots elongations. Translated to the ELT observing at zenith, elongations as long as 23.5 arcseconds must be accommodated, corresponding to a field of view of 16.3 arcseconds if the most elongated spots are put in the diagonal of the subaperture.
1958. Cancer cluster 1.4GHz continuum sources
ID:
ivo://CDS.VizieR/J/ApJ/317/102
Title:
Cancer cluster 1.4GHz continuum sources
Short Name:
J/ApJ/317/102
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report on 1.4GHZ continuum observations for 11 VLA fields, using the D-configuration, which contain the A group of the Cancer Cluster. Sixteen Zwicky spiral galaxies in the Cancer Cluster were detected, but no ellipticals. We corroborate the finding that spiral galaxies with close companions tend to have enhanced radio emission. Over 200 continuum sources beyond the Cancer Cluster are tabulated. The spectral index (relative to 610MHz) is given for many of the sources, including some of the Zwicky galaxies. There is a suggestion for a nonuniform number surface-density distribution of the sources, not correlated with the Cancer Cluster. Possible predictions of such nonuniformities, from assumptions on " super-superclusters," are discussed.
1959. 4C52.37 and 3C 293 parsec-scale HI outflows
ID:
ivo://CDS.VizieR/J/A+A/647/A63
Title:
4C52.37 and 3C 293 parsec-scale HI outflows
Short Name:
J/A+A/647/A63
Date:
21 Oct 2021
Publisher:
CDS
Description:
Massive outflows of neutral atomic hydrogen (HI) have been observed in absorption in a number of radio galaxies and are considered a signature of active galactic nucleus (AGN) feedback. These outflows on kiloparsec scales have not been investigated in great detail as they require high-angular-resolution observations to be spatially resolved. In some radio AGN, they are likely to be the result of the radio jets interacting with the interstellar medium. We have used the global very-long-baseline-interferometry (VLBI) array to map the HI outflow in a small sample of young and restarted radio galaxies that we previously observed with the Very Large Array (VLA) and the Westerbork Synthesis Radio Telescope (WSRT) at a lower resolution. Here we report on our findings for 4C 52.37 and 3C 293 and we discuss the sample including the previously published 4C 12.50 and 3C 236. For 4C 52.37, we present the first ever HI VLBI observations, which recovered the majority of the outflowing HI gas in the form of clouds toward the central 100pc of the AGN. The clouds are blueshifted by up to ~600km/s with respect to the systemic velocity. 3C 293 is largely resolved out in our VLBI observation, but toward the VLBI core we detect some outflowing HI gas blueshifted with respect to the systemic velocity by up to ~300km/s. We also find indications of outflowing gas toward the other parts of the western lobe suggesting that the HI outflow is extended. Overall, we find that the fraction of HI gas recovered by our VLBI observations varies significantly within our sample, ranging from complete (4C 12.50) to marginal (3C 293). However, in all cases we find evidence for a clumpy structure of both the outflowing and the quiescent gas, consistent with predictions from numerical simulations. All the outflows include at least a component of relatively compact clouds with masses in the range of 10^4^-10^5^M_{sun}_. The outflowing clouds are often already observed at a few tens of parsecs (in projection) from the core. We find indications that the HI outflow might have a diffuse component, especially in larger sources. Our results support the interpretation that we observe these AGNs at different stages in the evolution of the interaction between the jet and the interstellar medium and this is reflected in the properties of the outflowing gas as predicted by numerical simulations.
1960. CANDELS galaxy structure classification
ID:
ivo://CDS.VizieR/J/MNRAS/458/963
Title:
CANDELS galaxy structure classification
Short Name:
J/MNRAS/458/963
Date:
21 Oct 2021
Publisher:
CDS
Description:
Important but rare and subtle processes driving galaxy morphology and star formation may be missed by traditional spiral, elliptical, irregular or Sersic bulge/disc classifications. To overcome this limitation, we use a principal component analysis (PCA) of non-parametric morphological indicators (concentration, asymmetry, Gini coefficient, M_20_, multimode, intensity and deviation) measured at rest-frame B band (corresponding to HST/WFC3 F125W at 1.4<z<2) to trace the natural distribution of massive (>10^10^M_{sun}_) galaxy morphologies. PCA quantifies the correlations between these morphological indicators and determines the relative importance of each. The first three principal components (PCs) capture ~75 per cent of the variance inherent to our sample. We interpret the first PC as bulge strength, the second PC as dominated by concentration and the third PC as dominated by asymmetry. Both PC1 and PC2 correlate with the visual appearance of a central bulge and predict galaxy quiescence. PC1 is a better predictor of quenching than stellar mass, as good as other structural indicators (Sersic-n or compactness). We divide the PCA results into groups using an agglomerative hierarchical clustering method. Unlike Sersic, this classification scheme separates compact galaxies from larger, smooth protoelliptical systems, and star-forming disc-dominated clumpy galaxies from star-forming bulge-dominated asymmetric galaxies. Distinguishing between these galaxy structural types in a quantitative manner is an important step towards understanding the connections between morphology, galaxy assembly and star formation.

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