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J/A+A/607/A48       AGN data and absorption-line measurements  (Richter+, 2017)

An HST/COS legacy survey of high-velocity ultraviolet absorption in the Milky Way's circumgalactic medium and the Local Group. Richter P., Nuza S.E., Fox A.J., Wakker B.P., Ben Bekhti N., Fechner C., Wendt M., Howk J.C., Muzahid S., Ganguly R., Charlton J. <Astron. Astrophys. 607, A48 (2017)> =2017A&A...607A..48R (SIMBAD/NED BibCode)
ADC_Keywords: QSOs; Positional data; Spectroscopy; Equivalent widths Keywords: Galaxy: halo - Galaxy: evolution - ISM: kinematics and dynamics- techniques: spectroscopic - ultraviolet: ISM Abstract: The Milky Way is surrounded by large amounts of diffuse gaseous matter that connects the stellar body of our Galaxy with its large-scale Local Group (LG) environment. To characterize the absorption properties of this circumgalactic medium (CGM) and its relation to the LG we present the so-far largest survey of metal absorption in Galactic high-velocity clouds (HVCs) using archival ultraviolet (UV) spectra of extragalactic background sources. The UV data are obtained with the Cosmic Origins Spectrograph (COS) onboard the Hubble Space Telescope (HST) and are supplemented by 21cm radio observations of neutral hydrogen. Along 270 sightlines we measure metal absorption in the lines of SiII, SiIII, CII, and CIV and associated HI 21cm emission in HVCs in the velocity range |vLSR|=100-500km/s. With this unprecedented large HVC sample we were able to improve the statistics on HVC covering fractions, ionization conditions, small-scale structure, CGM mass, and inflow rate. For the first time, we determine robustly the angular two point correlation function of the high-velocity absorbers, systematically analyze antipodal sightlines on the celestial sphere, and compare the HVC absorption characteristics with that of Damped Lyman alpha absorbers (DLAs) and constrained cosmological simulations of the LG (CLUES project). The overall sky-covering fraction of high-velocity absorption is 77±6 percent for the most sensitive ion in our survey, SiIII, and for column densities log N(SiIII)>12.1. This value is 4-5 times higher than the covering fraction of 21 cm neutral hydrogen emission at log N(HI)>18.7 along the same lines of sight, demonstrating that the Milky Way's CGM is multi-phase and predominantly ionized. The measured equivalent-width ratios of SiII, SiIII, CII, and CIV are inhomogeneously distributed on large and small angular scales, suggesting a complex spatial distribution of multi-phase gas that surrounds the neutral 21cm HVCs. We estimate that the total mass and accretion rate of the neutral and ionized CGM traced by HVCs is MHVC>3.0x109M and dMHVC/dt>6.1M/yr, where the Magellanic Stream (MS) contributes with more than 90 percent to this mass/mass-flow. If seen from an external vantage point, the Milky Way disk plus CGM would appear as a DLA that would exhibit for most viewing angles an extraordinary large velocity spread of dv=400-800km/s, a result of the complex kinematics of the Milky Way CGM that is dominated by the presence of the MS. We detect a velocity dipole of high-velocity absorption at low/high galactic latitudes that we associate with LG gas that streams to the LG barycenter. This scenario is supported by the gas kinematics predicted from the LG simulations. Our study confirms previous results, indicating that the Milky Way CGM contains sufficient gaseous material to feed the Milky Way disk over the next Gyr at a rate of a few solar masses per year, if the CGM gas can actually reach the MW disk. We demonstrate that the CGM is composed of discrete gaseous structures that exhibit a large-scale kinematics together with small-scale variations in physical conditions. The MS clearly dominates both the cross section and mass flow of high-velocity gas in the Milky Way's CGM. The possible presence of high-velocity LG gas underlines the important role of the local cosmological environment in the large-scale gas-circulation processes in and around the Milky Way. Description: Names and positions for 270 QSOs are provided in Table A.1. Table A.2 summarizes the absorption-line measurements for high-velocity absorption along 187 sightlines including absorption velocities, equivalent-widths, and column densities for various different ions. Table A.4 lists the hydrogen column densities for the high-velocity absorbers. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 54 270 QSO names and Galactic coordinates tablea2.dat 114 1049 Absorption-line measurements in HVC tablea4.dat 68 187 Hydrogen column densities in HVCs
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
3- 5 I3 --- No Row number 7- 33 A27 --- Name QSO name 41- 45 F5.1 deg GLON Galactic longitude 50- 54 F5.1 deg GLAT Galactic latitude
Byte-by-byte Description of file: tablea2.dat
Bytes Format Units Label Explanations
2- 5 I4 --- No Row number 7- 33 A27 --- Name QSO name (COS) 38- 42 A5 --- Ion Ion 48- 53 F6.1 0.1nm lambda0 Laboratory wavelength 58- 60 I3 --- S/N Signal-to-noise per resolution element 66- 69 I4 km/s vmin Lower velocity limit of HVC absorption 75- 78 I4 km/s vmax Upper velocity limit of HVC absorption 83 A1 --- Flag [t] Flag for tentative HVC detection 84- 87 I4 0.1pm W ? Equivalent width 94- 96 I3 0.1pm e_W ? Sigma equivalent width 100 A1 --- l_logN Limit flag on logN 101-105 F5.2 [cm/2] logN ? Logarithmic column density (or limit) 111-114 F4.2 [cm/2] e_logN ? Sigma logarithmic column density
Byte-by-byte Description of file: tablea4.dat
Bytes Format Units Label Explanations
2- 4 I3 --- No Row number 6- 32 A27 --- Name QSO name (COS) 38- 41 I4 km/s vHVC Center velocity of HVC absorption/emission 45 A1 --- l_logN(HI) Limit flag on logN(HI) 46- 50 F5.2 [cm/s2] logN(HI) Logarithmic column density (or limit) of HI 54 A1 --- l_logN(H) Limit flag on logN(H) 55- 59 F5.2 [cm/s2] logN(H) Logarithmic column density (or limit) of H 63 A1 --- l_logf(HI) Limit flag on logf(HI) 64- 68 F5.2 [cm/s2] logf(HI) Logarithmic neutral hydrogen fraction (or limit)
Acknowledgements: Philipp Richter, prichter(at)astro.physik.uni-potsdam.de
(End) P. Richter [Univ. Potsdam, Germany], P. Vannier [CDS] 20-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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