Chlorine-bearing molecules in molecular absorbers at intermediate redshifts

Wallström, Sofia; Müller, S.; Roueff, E.; Gal, Romane Le; Black, J. H.; Gérin, M.

doi:10.1051/0004-6361/201935860

Cited by 19 publications

(9 citation statements)

References 51 publications

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“…2. Conversely, gas-phase molecules that reach the upper layers of the disk are subject to the harsh, PDR-like radiation environment of the star and Whiteoak et al (1980) [2] Churchwell et al (1977) [3] Martin & Ho (1979) [4] Mauersberger et al (1990) [5] Henkel et al (1988) [6] Stark & Wolff (1979) [7] Gardner & Whiteoak (1974) [8] Tercero et al (2020) [9] Magain & Gillet (1987) [10] Rickard et al (1977) [11] Nguyen-Q- Rieu et al (1991) [12] Muller et al (2011) [13] Weliachew (1971) [14] Mauersberger et al (1995) [15] Martín et al (2006) [16] Rickard et al (1975) [17] Matsuura et al (2002) [18] Thompson et al (1978) [19] Heikkilä et al (1999) [20] ) [21] Aladro et al (2015 [22] Seaquist & Bell (1986) [23] Henkel & Bally (1985) [24] Johansson (1991) [25] Petuchowski & Bennett (1992) [26] Martín et al (2003) [27] van der Tak et al (2008) [28] Sage & Ziurys (1995) [29] García-Burillo et al (2002) [30] Welty et al (2013) [31] Muller et al (2013) [32] Usero et al (2004) [33] Wallström et al (2019) [34] González-Alfonso et al (2004 [35] [36] Fuente et al (2006) [37] Geballe et al (2006) [38] van der Werf et al (2010) [39] Rangwala et al (2011) [40] Monje et al (2011) [41] <...>…”

Section: Often Narrow Ranges Of Physical Environments Con-mentioning

confidence: 99%

2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules

McGuire

2018

ApJS

397

290

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To date, 204 individual molecular species, comprised of 16 different elements, have been detected in the interstellar and circumstellar medium by astronomical observations. These molecules range in size from two atoms to seventy, and have been detected across the electromagnetic spectrum from cmwavelengths to the ultraviolet. This census presents a summary of the first detection of each molecular species, including the observational facility, wavelength range, transitions, and enabling laboratory spectroscopic work, as well as listing tentative and disputed detections. Tables of molecules detected in interstellar ices, external galaxies, protoplanetary disks, and exoplanetary atmospheres are provided. A number of visual representations of this aggregate data are presented and briefly discussed in context.

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Section: Often Narrow Ranges Of Physical Environments Con-mentioning

confidence: 99%

2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules

McGuire

2018

ApJS

397

290

View full text Add to dashboard Cite

show abstract

“…Based on observations of B 0281+357 with the Plateau de Bure interferometer, we estimate an H 2 column density of 8 × 10 21 cm −2 (Wallström et al 2016), which would imply an abundance ratio 7 LiH/H 2 ∼ 10 −10 . Since the overall chemical and physical properties of the absorbing gas in the two molecular absorbers toward B 0218+357 and PKS 1830−211 are comparable (see, e.g., Wallström et al 2019), it is difficult to reconcile such several orders of magnitude different relative abundance of LiH between them. It is however likely that these tentative detections were due to spurious arti- facts 6 .…”

Section: Ratio A/bmentioning

confidence: 99%

Detection of deuterated molecules, but not of lithium hydride, in the z = 0.89 absorber toward PKS 1830−211

Müller

Roueff

Black

et al. 2020

A&A

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Deuterium and lithium are light elements of high cosmological and astrophysical importance. In this work we report the first detection of deuterated molecules and a search for lithium hydride, 7LiH, at redshift z = 0.89 in the spiral galaxy intercepting the line of sight to the quasar PKS 1830−211. We used ALMA to observe several submillimeter lines of ND, NH2D, and HDO, and their related isotopomers NH2, NH3, and H218O, in absorption against the southwest image of the quasar, allowing us to derive XD/XH abundance ratios. The absorption spectra mainly consist of two distinct narrow velocity components for which we find remarkable differences. One velocity component shows XD/XH abundances that is about 10 times larger than the primordial elemental D/H ratio, and no variability of the absorption profile during the time span of our observations. In contrast, the other component shows a stronger deuterium fractionation. Compared to the first component, this second component has XD/XH abundances that are 100 times larger than the primordial D/H ratio, a deepening of the absorption by a factor of two within a few months, and a rich chemical composition, with relative enhancements of N2H+, CH3OH, SO2 and complex organic molecules. We therefore speculate that this component is associated with the analog of a Galactic dark cloud, while the first component is likely more diffuse. Our search for the 7LiH (1–0) line was unsuccessful and we derive an upper limit 7LiH/H2 = 4 × 10−13 (3σ) in the z = 0.89 absorber toward PKS 1830−211. Besides, with ALMA archival data, we could not confirm the previous tentative detections of this line in the z = 0.68 absorber toward B 0218+357; we derive an upper limit 7LiH/H2 = 5 × 10−11 (3σ), although this is less constraining than our limit toward PKS 1830−211. We conclude that, as in the Milky Way, only a tiny fraction of lithium nuclei are possibly bound in LiH in these absorbers at intermediate redshift.

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“…Based on observations of B 0281+357 with the Plateau de Bure interferometer, we estimate an H 2 column density of 8 × 10 21 cm −2 (Wallström et al, 2016), which would imply an abundance ratio 7 LiH/H 2 ∼ 10 −10 . Since the overall chemical and physical properties of the absorbing gas in the two molecular absorbers toward B 0218+357 and PKS 1830−211 are comparable (see, e.g., Wallström et al 2019), it is difficult to reconcile such several orders of magnitude different relative abundance of LiH between them. It is however likely that these tentative detections were due to spurious artifacts 6 .…”

Section: Non-detection Of 7 Lihmentioning

confidence: 99%

Detection of deuterated molecules, but not of lithium hydride, in the z=0.89 absorber toward PKS1830-211

Muller,

Roueff,

Black

et al. 2020

Preprint

Self Cite

View full text Add to dashboard Cite

Deuterium and lithium are light elements of high cosmological and astrophysical importance. In this work we report the first detection of deuterated molecules and a search for lithium hydride, 7 LiH, at redshift z=0.89 in the spiral galaxy intercepting the line of sight to the quasar PKS 1830−211. We used ALMA to observe several submillimeter lines of ND, NH2D, and HDO, and their related isotopomers NH2, NH3, and H 18 2 O, in absorption against the southwest image of the quasar, allowing us to derive XD/XH abundance ratios. The absorption spectra mainly consist of two distinct narrow velocity components for which we find remarkable differences. One velocity component shows XD/XH abundances that is about 10 times larger than the primordial elemental D/H ratio, and no variability of the absorption profile during the time span of our observations. In contrast, the other component shows a stronger deuterium fractionation. Compared to the first component, this second component has XD/XH abundances that are 100 times larger than the primordial D/H ratio, a deepening of the absorption by a factor of two within a few months, and a rich chemical composition, with relative enhancements of N2H + , CH3OH, SO2 and complex organic molecules. We therefore speculate that this component is associated with the analog of a Galactic dark cloud, while the first component is likely more diffuse. Our search for the 7 LiH (1-0) line was unsuccessful and we derive an upper limit 7 LiH/H2 = 4 × 10 −13 (3σ) in the z=0.89 absorber toward PKS 1830−211. Besides, with ALMA archival data, we could not confirm the previous tentative detections of this line in the z=0.68 absorber toward B 0218+357; we derive an upper limit 7 LiH/H2 = 5 × 10 −11 (3σ), although this is less constraining than our limit toward PKS 1830−211. We conclude that, as in the Milky Way, only a tiny fraction of lithium nuclei are possibly bound in LiH in these absorbers at intermediate redshift.

show abstract

Chlorine-bearing molecules in molecular absorbers at intermediate redshifts

Cited by 19 publications

References 51 publications

2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules

2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules

Detection of deuterated molecules, but not of lithium hydride, in the z = 0.89 absorber toward PKS 1830−211

Detection of deuterated molecules, but not of lithium hydride, in the z=0.89 absorber toward PKS1830-211

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