2017A&A...606A.109M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:45:35

2017A&A...606A.109M - Astronomy and Astrophysics, volume 606A, 109-109 (2017/10-1)

Detection of CH+, SH+, and their 13C- and 34S-isotopologues toward PKS 1830-211.

MULLER S., MULLER H.S.P., BLACK J.H., GERIN M., COMBES F., CURRAN S., FALGARONE E., GUELIN M., HENKEL C., MARTIN S., MENTEN K.M., ROUEFF E., AALTO S., BEELEN A., WIKLIND T. and ZWAAN M.A.

Abstract (from CDS):

The z=0.89 molecular absorber toward PKS 1830-211 provides us with the opportunity to probe the chemical and physical properties of the interstellar medium in the disk of a galaxy at a look-back time of half the present age of the Universe. Recent ALMA observations of hydrides have unveiled the multi-phase composition of this source's interstellar medium along two absorbing sightlines. Here, we report ALMA observations of CH+ and SH+, and of their 13C- and 34S-isotopologues, as potential tracers of energetic processes in the interstellar medium. CH+ and 13CH+ are detected toward both images of PKS 1830-211, CH+ showing the deepest and broadest absorption among all species observed so far. The CH+/13CH+ abundance ratio is ∼100 in the south-west line of sight. This value is larger than any previous 12CX/13CX ratios determined from other species toward this source and suggests either that the latter might be affected by fractionation or that CH+ might be tracing a different gas component. Toward the north-east image, we find an even larger value of CH+/13CH+, 146±43, although with a large uncertainty. This sightline intercepts the absorber at a larger galactocentric radius than the southwestern one, where material might be less processed in stellar nucleosynthesis. In contrast to CH+ and its 13C isotopologue, SH+ and 34SH+ are only detected on the south-west sightline. These are the first detections of extragalactic SH+ and interstellar 34SH+. The spectroscopic parameters of SH+ are reevaluated and improved rest frequencies of 34SH+ are obtained. The CH+/SH+ column density ratios show a large difference between the two lines of sight: ∼25 and >600 toward the SW and NE image, respectively. We are not able to shed light on the formation process of CH+ and SH+ with these data, but the differences between the two sightlines toward PKS 1830-211 suggest that their absorptions arise from gas with a molecular fraction of >=10%, with SH+ tracing significantly higher molecular fractions than CH+.

Abstract Copyright: © ESO, 2017

Journal keyword(s): quasars: absorption lines - quasars: individual: PKS 1830-211 - galaxies: ISM - galaxies: abundances - ISM: molecules - radio lines: galaxies - radio lines: galaxies

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 329 0
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
3 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
4 ESO 428-14 Sy2 07 16 31.2067043371 -29 19 28.898984517   13.28 13.52 11.61   ~ 216 4
5 SN 2008fp SN* 07 16 32.60 -29 19 31.7           SNIa 51 1
6 SN 2014J SN* 09 55 42.12 +69 40 25.9           SNIa 317 1
7 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5336 6
8 SN 2006X SN* 12 22 53.93 +15 48 32.0     15.3     SNIa 280 1
9 M 100 AGN 12 22 54.9318850854 +15 49 20.294302163 10.04 10.05 9.35     ~ 1647 2
10 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3999 3
11 SN 1986G SN* 13 25 36.46 -43 01 53.6   12.45 11.44     SNIapec 384 1
12 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11540 0
13 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1909 1
14 QSO B1830-211 QSO 18 33 39.92 -21 03 39.9     18.70 21   ~ 549 6
15 QSO B1921-293 BLL 19 24 51.05595514 -29 14 30.1210524   18.71 18.21 15.07   ~ 689 0
16 NAME Local Group GrG ~ ~           ~ 6973 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:45:35

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