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91. Absorption in multiphase circumgalactic medium
ID:
ivo://CDS.VizieR/J/MNRAS/445/2061
Title:
Absorption in multiphase circumgalactic medium
Short Name:
J/MNRAS/445/2061
Date:
21 Oct 2021
Publisher:
CDS
Description:
This paper presents an absorption-line study of the multiphase circumgalactic medium (CGM) based on observations of Ly{alpha}, CII, CIV, SiII, SiIII, and SiIV absorption transitions in the vicinities of 195 galaxies at redshift z<0.176. The galaxy sample is established based on a cross-comparison between public galaxy and quasi-stellar object (QSO) survey data and is characterized by a median redshift of <z>=0.041, a median projected distance of <d>=362kpc to the sightline of the background QSO, and a median stellar mass of log(M_star_/M_{sun}_)=9.7+/-1.1. Comparing the absorber features identified in the QSO spectra with known galaxy properties has led to strong constraints for the CGM absorption properties at z<~0.176. First, abundant hydrogen gas is observed out to d~500kpc, well beyond the dark matter halo radius R_h_ of individual galaxies, with a mean covering fraction of ~60 percent. In contrast, no heavy elements are detected at d>~0.7R_h_ from either low-mass dwarfs or high-mass galaxies. The lack of detected heavy elements in low- and high-ionization states suggests that either there exists a chemical enrichment edge at d~0.7R_h_ or gaseous clumps giving rise to the observed absorption lines cannot survive at these large distances. Considering all galaxies at d>R_h_ leads to a strict upper limit for the covering fraction of heavy elements of ~3% (at a 95% confidence level) over d=(1-9)R_h_. At d<R_h_, differential covering fraction between low- and high-ionization gas is observed, suggesting that the CGM becomes progressively more ionized from d<0.3R_h_ to larger distances. Comparing CGM absorption observations at low and high redshifts shows that at a fixed fraction of R_h_ the CGM exhibits stronger mean absorption at z=2.2 than at z~0, and that the distinction is most pronounced in low-ionization species traced by CII and SiII absorption lines. We discuss possible pseudo-evolution of the CGM as a result of misrepresentation of halo radius, and present a brief discussion on the implications of these findings.
92. Absorption lines in 21 Lyn A-type star
ID:
ivo://CDS.VizieR/J/ApJS/239/19
Title:
Absorption lines in 21 Lyn A-type star
Short Name:
J/ApJS/239/19
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a catalog of absorption lines in the z', Y, and J bands that we identified in 21 Lyn, a slowly rotating A0.5V star. We detected 155 absorption features in the high-resolution (0.90-1.35um, R=28000) spectrum obtained with the WINERED spectrograph after the telluric absorption was carefully removed using a spectrum of a B-type star as a telluric standard. With a visual comparison with synthetic spectra, we compiled a catalog of 219 atomic lines for the 155 features, some of which are composed of multiple fine structure lines. The high-quality WINERED spectrum enabled us to detect a large number of weak lines down to ~1% in depth, which are identified for an A-type star for the first time. The catalog includes the lines of H, C, N, O, Mg, Al, Si, S, Ca, Fe, and Sr. These new lines are expected to be useful for spectral classification and chemical abundance analyses, while the line catalog is useful for observers who plan to use A-type stars as telluric standards because it is necessary to distinguish between stellar lines and telluric absorption lines in high-resolution spectra. ASCII versions of the spectra are available in the online version of the journal.
93. Absorption lines in QSO 0000-2619
ID:
ivo://CDS.VizieR/J/A+A/318/347
Title:
Absorption lines in QSO 0000-2619
Short Name:
J/A+A/318/347
Date:
21 Oct 2021
Publisher:
CDS
Description:
We give the list of absorption lines in the high resolution (FWHM=13 km/s) spectrum of the z=4.12 QSO 0000-2619. The first table contains the lines of the Lyman-alpha forest, while in the second table the lines of the metal systems are listed.
94. Absorption-line strengths in Coma galaxies
ID:
ivo://CDS.VizieR/J/MNRAS/386/715
Title:
Absorption-line strengths in Coma galaxies
Short Name:
J/MNRAS/386/715
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present stellar population parameters of 12 elliptical and S0 galaxies in the Coma cluster around and including the cD galaxy NGC 4874, based on spectra obtained using the Low Resolution Imaging Spectrograph on the Keck II Telescope. Our data are among the most precise and accurate absorption-line strengths yet obtained for cluster galaxies, allowing us to examine in detail the zero-point and scatter in the stellar population properties of Coma cluster early-type galaxies (ETGs).
95. Absorption-line systems in QSO spectra - CoALS
ID:
ivo://CDS.VizieR/J/A+A/412/707
Title:
Absorption-line systems in QSO spectra - CoALS
Short Name:
J/A+A/412/707
Date:
21 Oct 2021
Publisher:
CDS
Description:
Absorption lines and absorption-line systems (ALSs) observed in the spectra of QSOs contain fundamental information on distribution of matter between the observer and the QSO, and on physical processes in the Universe in different epochs of the cosmological evolution. The presented catalog contains a compilation of basic information on absorption-line systems (ALSs) in QSO spectra. The data are taken from publications available to the authors up to January 2002. The catalog includes, in particular, all the data of the catalogs by Junkkarinen et al. (1991ApJS...77..203J) and York et al. (1991MNRAS.250...24Y ). The catalog consists of table1.dat, table2.txt and the list of references in refs.dat file. The present catalog is also available at the site of the Dept. of Theor. Astrophys. of the Ioffe Physical Technical Institute: <www.ioffe.ru/astro/QC>
96. Absorption spectrum of SO up to 2.5THz
ID:
ivo://CDS.VizieR/J/ApJ/799/115
Title:
Absorption spectrum of SO up to 2.5THz
Short Name:
J/ApJ/799/115
Date:
21 Oct 2021
Publisher:
CDS
Description:
In order to obtain accurate terahertz center frequencies for SO and its isotopologues, we have studied the absorption spectrum of SO, ^34^SO, and ^33^SO up to 2.5THz using continuous-wave terahertz photomixing based on a frequency comb providing an accuracy down to 10kHz. Sulfur monoxide was produced in a radio frequency discharge of air in a cell containing pure sulfur. Together with the strong absorption signal of the main isotopologue, transitions of ^34^SO (^34^S: 4.21%) and ^33^SO (^33^S: 0.75%) were observed in natural abundance. The newly observed transitions constitute an extension of the observed rotational quantum numbers of the molecule toward higher N values, allowing an improvement of the molecular parameters for the three species. An isotopically invariant fit has been performed based on pure rotational and ro-vibrational transitions of all SO isotopologues, enabling their accurate line position prediction at higher frequencies. Thanks to this new set of parameters, it is now possible to predict with very high accuracy the frequencies of the ro-vibrational lines. This should enable the research of SO in the mid-IR using ground-based IR telescopes, space-based telescope archives (Infrared Space Observatory, Spitzer), and future space missions such as the James Webb Space Telescope. This set of parameters is particularly well adapted for the detection of SO lines in O-rich evolved stars or in molecular clouds in absorption against bright IR sources.
97. Absorption spectrum of the QSO PKS2126-158
ID:
ivo://CDS.VizieR/J/A+AS/127/217
Title:
Absorption spectrum of the QSO PKS2126-158
Short Name:
J/A+AS/127/217
Date:
21 Oct 2021
Publisher:
CDS
Description:
Spectra of the z_em_=3.268 quasar PKS 2126-158 have been obtained in the wavelength range 430-662nm with a resolution R=27000 and an average signal to noise ratio s/n=25 per resolution element. 12 metal absorption systems have been identified, two of which were previously unknown. All the lines shortward of the Lyman{alpha} emission not identified as due to metals have been fitted as Lyman{alpha} and Lyman{beta}. We reported statistical analysis of this sample of lines. In particular, the two-point correlation function for metal systems has been computed.
98. Absorption systems of HS 1700+6416
ID:
ivo://CDS.VizieR/J/A+A/294/377
Title:
Absorption systems of HS 1700+6416
Short Name:
J/A+A/294/377
Date:
21 Oct 2021
Publisher:
CDS
Description:
Ultraviolet observations of the high-redshift quasat HS 1700+6416 were obtained with the Faint Object Spectrograph (FOS) onboard the Hubble Space Telescope (HST) in the range 115-328nm, on 1991-12-13/14 and 1992-02-13/14 at a resolution R=1300. The identification of the numerous absoprtion lines provides evidence for 15 heavy-element absorption systems, among them 7 Lyman Limit systems (LLS).
99. Absorption toward PG 1116+215
ID:
ivo://CDS.VizieR/J/ApJS/155/351
Title:
Absorption toward PG 1116+215
Short Name:
J/ApJS/155/351
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present Hubble Space Telescope (HST) and Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the intergalactic absorption toward QSO PG 1116+215 in the 900-3000{AA} spectral region.
100. Absorption velocities for 21 super-luminous SNe Ic
ID:
ivo://CDS.VizieR/J/ApJ/845/85
Title:
Absorption velocities for 21 super-luminous SNe Ic
Short Name:
J/ApJ/845/85
Date:
21 Oct 2021
Publisher:
CDS
Description:
Super-luminous supernovae (SLSNe) are tremendously luminous explosions whose power sources and progenitors are highly debated. Broad-lined SNe Ic (SNe Ic-bl) are the only type of SNe that are connected with long-duration gamma-ray bursts (GRBs). Studying the spectral similarity and difference between the populations of hydrogen-poor SLSNe (SLSNe Ic) and of hydrogen-poor stripped-envelope core-collapse SNe, in particular SNe Ic and SNe Ic-bl, can provide crucial observations to test predictions of theories based on various power source models and progenitor models. In this paper, we collected all of the published optical spectra of 32 SLSNe Ic, 21 SNe Ic-bl, as well as 17 SNe Ic, quantified their spectral features, constructed average spectra, and compared them in a systematic way using new tools we have developed. We find that SLSNe Ic and SNe Ic-bl, including those connected with GRBs, have comparable widths for their spectral features and average absorption velocities at all phases. Thus, our findings strengthen the connection between SLSNe Ic and GRBs. In particular, SLSNe Ic have average FeII{lambda}5169 absorption velocities of -15000+/-2600km/s at 10 days after peak, which are higher than those of SNe Ic by ~7000km/s on average. SLSNe Ic also have significantly broader FeII{lambda}5169 lines than SNe Ic. Moreover, we find that such high absorption and width velocities of SLSNe Ic may be hard to explain with the interaction model, and none of the 13 SLSNe Ic with measured absorption velocities spanning over 10 days has a convincing flat velocity evolution, which is inconsistent with the magnetar model in one dimension. Lastly, we compare SN 2011kl, the first SN connected with an ultra-long GRB, with the mean spectrum of SLSNe Ic and of SNe Ic-bl.

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