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2841. The Hamburg/SAO Survey for ELGs. V.
ID:
ivo://CDS.VizieR/J/A+A/374/907
Title:
The Hamburg/SAO Survey for ELGs. V.
Short Name:
J/A+A/374/907
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the fifth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). The list is a result of follow-up spectroscopy conducted with the 2.2m CAHA and 4m Kitt Peak telescopes in 1999. The data of this snap-shot spectroscopy survey confirmed 166 emission-line objects out of 209 observed candidates and allowed their quantitative spectral classification and redshift determination. We could classify 98 emission-line objects as BCG/HII galaxies or probable BCGs, 5 as QSOs, 3 as Seyfert galaxies, 2 as super-associations in subluminous spiral galaxies. 25 low-excitation objects were classified as starburst nuclei (SBN), 24 as dwarf amorphous nuclei starburst galaxies (DANS) and 3 as LINERs. Due to low signal-to-noise ratio we could not classify 6 ELGs. Furthermore, for another 4 galaxies we did not detect any significant emission lines. For 131 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. For the remaining 30 previously known ELGs we give either improved data of the line intensities or some independent measurements.
2842. The Hawai K-band survey. III.
ID:
ivo://CDS.VizieR/J/ApJS/94/461
Title:
The Hawai K-band survey. III.
Short Name:
J/ApJS/94/461
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present spectra and multicolor (B,I,K) data for near-infrared (K) selected spatially complete magnitude limited (K<20) galaxy samples from the Hawaii Survey. The redshift identification of the sample of 298 galaxies is substantially complete to a B magnitude of 26 and an I magnitude of 22.5, and identification of observed galaxies ranges from nearly 100% completeness at K<18 to ~70% completeness at K=19-20. We note that many of the unidentified objects appear to be red (I-K) objects which are flat in the optical and spectroscopically featureless. Strengths of spectral-line features and breaks are tabulated for the 262 galaxies with reasonably secure redshifts. The measured redshifts nearly all fall at z<1, with the exception of a compact absorption-line object at z=2.35. At K>=18, the redshift distribution is well fitted by a model with no luminosity evolution, implying that from the K-band Hubble diagram, the Hubble constant can vary at most by 10% over the redshift range from z~0.025 to 0.25, and that positive luminosity evolution at any significant level between z=0 and z=1 is ruled out. However, the evolution of both the emission-line strengths and the 4000{AA} break indicates that galaxies were undergoing significantly more star formation at z=1 than at the present time.
2843. The HeCS-omnibus catalog: SDSS & MMT sp. obs.
ID:
ivo://CDS.VizieR/J/ApJ/891/129
Title:
The HeCS-omnibus catalog: SDSS & MMT sp. obs.
Short Name:
J/ApJ/891/129
Date:
21 Oct 2021
Publisher:
CDS
Description:
We explore connections between brightest cluster galaxies (BCGs) and their host clusters. We first construct a HeCS-omnibus cluster sample including 227 galaxy clusters within 0.02<z<0.30; the total number of spectroscopic members from MMT/Hectospec and SDSS observations is 52325. Taking advantage of the large spectroscopic sample, we compute physical properties of the clusters including the dynamical mass and cluster velocity dispersion ({sigma}_cl_). We also measure the central stellar velocity dispersion of the BCGs ({sigma}_*,BCGs_) to examine the relation between BCG velocity dispersion and cluster velocity dispersion for the first time. The observed relation between BCG velocity dispersion and the cluster velocity dispersion is remarkably tight. Interestingly, the {sigma}_*,BCG_/{sigma}_cl_ ratio decreases as a function of {sigma}_cl_ unlike the prediction from the numerical simulation of Dolag+ (2010MNRAS.405.1544D). The trend in {sigma}_*,BCG_/{sigma}_cl_ suggests that BCG formation is more efficient in lower mass halos.
2844. The HectoMAP cluster survey. I.
ID:
ivo://CDS.VizieR/J/ApJ/856/172
Title:
The HectoMAP cluster survey. I.
Short Name:
J/ApJ/856/172
Date:
21 Oct 2021
Publisher:
CDS
Description:
We use the dense HectoMAP redshift survey to explore the properties of 104 redMaPPer cluster candidates. The redMaPPer systems in HectoMAP cover the full range of richness and redshift (0.08<z<0.60). Fifteen of the systems included in the Subaru/Hyper Suprime-Cam public data release are bona fide clusters. The median number of spectroscopic members per cluster is ~20. We include redshifts of 3547 member candidates listed in the redMaPPer catalog whether they are cluster members or not. We evaluate the redMaPPer membership probability spectroscopically. The purity (number of real systems) in redMaPPer exceeds 90% even at the lowest richness. Three massive galaxy clusters (M~2x10^13^M_{sun}_) associated with X-ray emission in the HectoMAP region are not included in the public redMaPPer catalog with {lambda}_rich_>20, because they lie outside the cuts for this catalog.
2845. The HectoMAP cluster survey. II. X-ray clusters
ID:
ivo://CDS.VizieR/J/ApJ/855/100
Title:
The HectoMAP cluster survey. II. X-ray clusters
Short Name:
J/ApJ/855/100
Date:
21 Oct 2021
Publisher:
CDS
Description:
We apply a friends-of-friends algorithm to the HectoMAP redshift survey and cross-identify associated X-ray emission in the ROSAT All-Sky Survey data (RASS). The resulting flux-limited catalog of X-ray cluster surveys is complete to a limiting flux of ~3x10^-13^erg/s/cm^2^ and includes 15 clusters (7 newly discovered) with redshifts z<=0.4. HectoMAP is a dense survey (~1200 galaxies deg^-2^) that provides ~50 members (median) in each X-ray cluster. We provide redshifts for the 1036 cluster members. Subaru/Hyper Suprime-Cam imaging covers three of the X-ray systems and confirms that they are impressive clusters. The HectoMAP X-ray clusters have an LX-{sigma}cl scaling relation similar to that of known massive X-ray clusters. The HectoMAP X-ray cluster sample predicts ~12000+/-3000 detectable X-ray clusters in RASS to the limiting flux, comparable with previous estimates.
2846. The Hopkins Ultraviolet Telescope (HUT)
ID:
ivo://CDS.VizieR/VI/103
Title:
The Hopkins Ultraviolet Telescope (HUT)
Short Name:
VI/103
Date:
21 Oct 2021
Publisher:
CDS
Description:
The Hopkins Ultraviolet Telescope HUT was one of three ultraviolet instruments of the ASTRO-1 mission flown on the space shuttle Columbia during 2-10 December 1990. 106 spectrophotometric observations of 77 targets were obtained in the far-UV (i.e., 912-1850{AA}) at a resolution of ~3{AA}. A few sources were observed in the 415-912{AA} region with a 1.5{AA} resolution. The same three instruments were later flown on the space shuttle Endeavour from 3-17 March 1995 as part of the ASTRO-2 mission. During the longer ASTRO-2 mission, 385 observations of 265 targets were obtained.
2847. The hot Jupiter Kepler-13Ab planet's occultation
ID:
ivo://CDS.VizieR/J/ApJ/788/92
Title:
The hot Jupiter Kepler-13Ab planet's occultation
Short Name:
J/ApJ/788/92
Date:
21 Oct 2021
Publisher:
CDS
Description:
Kepler-13Ab (= KOI-13.01) is a unique transiting hot Jupiter. It is one of very few known short-period planets orbiting a hot A-type star, making it one of the hottest planets currently known. The availability of Kepler data allows us to measure the planet's occultation (secondary eclipse) and phase curve in the optical, which we combine with occultations observed by warm Spitzer at 4.5 {mu}m and 3.6 {mu}m and a ground-based occultation observation in the K_s_ band (2.1 {mu}m). We derive a day-side hemisphere temperature of 2750+/-160 K as the effective temperature of a black body showing the same occultation depths. Comparing the occultation depths with one-dimensional planetary atmosphere models suggests the presence of an atmospheric temperature inversion. Our analysis shows evidence for a relatively high geometric albedo, A_g_=0.33_-0.06_^+0.04^. While measured with a simplistic method, a high A_g_ is supported also by the fact that the one-dimensional atmosphere models underestimate the occultation depth in the optical. We use stellar spectra to determine the dilution, in the four wide bands where occultation was measured, due to the visual stellar binary companion 1.15"+/-0.05" away. The revised stellar parameters measured using these spectra are combined with other measurements, leading to revised planetary mass and radius estimates of M_p_=4.94-8.09 M_J_ and R_p_=1.406+/-0.038 R_J_. Finally, we measure a Kepler midoccultation time that is 34.0+/-6.9 s earlier than expected based on the midtransit time and the delay due to light-travel time and discuss possible scenarios.
2848. The ISO-SWS post-helium atlas
ID:
ivo://CDS.VizieR/J/A+A/390/1033
Title:
The ISO-SWS post-helium atlas
Short Name:
J/A+A/390/1033
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present an atlas of near-infrared spectra (2.36{mu}m-4.1{mu}m) of ~300 stars at moderate resolution ({lambda}/{delta}{lambda}~1500-2000). The spectra were recorded using the Short-Wavelength Spectrometer aboard the Infrared Space Observatory (ISO-SWS). The bulk of the observations were performed during a dedicated observation campaign after the liquid helium depletion of the ISO satellite, the so-called post-helium programme. This programme was aimed at extending the MK-classification to the near-infrared.
2849. The kinematics of the C II {lambda}6578 line in PNe
ID:
ivo://CDS.VizieR/J/AJ/153/140
Title:
The kinematics of the C II {lambda}6578 line in PNe
Short Name:
J/AJ/153/140
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present spectroscopic observations of the C II {lambda}6578 permitted line for 83 lines of sight in 76 planetary nebulae at high spectral resolution, most of them obtained with the Manchester Echelle Spectrograph on the 2.1 m telescope at the Observatorio Astronomico Nacional on the Sierra San Pedro Martir. We study the kinematics of the C II {lambda}6578 permitted line with respect to other permitted and collisionally excited lines. Statistically, we find that the kinematics of the C II {lambda}6578 line are not those expected if this line arises from the recombination of C^2+^ ions or the fluorescence of C^+^ ions in ionization equilibrium in a chemically homogeneous nebular plasma, but instead its kinematics are those appropriate for a volume more internal than expected. The planetary nebulae in this sample have well-defined morphology and are restricted to a limited range in H{alpha} line widths (no large values) compared to their counterparts in the Milky Way bulge; both these features could be interpreted as the result of young nebular shells, an inference that is also supported by nebular modeling. Concerning the long-standing discrepancy between chemical abundances inferred from permitted and collisionally excited emission lines in photoionized nebulae, our results imply that multiple plasma components occur commonly in planetary nebulae.
2850. The LickX Spectra library
ID:
ivo://CDS.VizieR/J/A+A/561/A36
Title:
The LickX Spectra library
Short Name:
J/A+A/561/A36
Date:
21 Oct 2021
Publisher:
CDS
Description:
Collections of stellar spectra, often called stellar libraries, are useful in a variety of applications in the field of stellar populations. This is an attempt to improve the much-used Lick library of stellar spectra by removing jitter from the wavelength scale via cross-correlation, and calling the result the LickX library.

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