The warm, the excited, and the molecular gas: GRB 121024A shining through its star-forming galaxy★

Friis, M.; De, A.; Krühler, T.; Fynbo, J. P. U.; Ledoux, C.; Vreeswijk, P. M.; Watson, Derrick G.; Malesani, D.; Gorosabel, J.; Starling, R. L. C.; Jakobsson, P.; Varela, K.; Wiersema, K.; Drachmann, A. Paaske; Trotter, A.; Thöne, C. C.; Postigo, A. de Ugarte; D’Elia, V.; Elliott, J.; Maturi, M.; Goldoni, P.; Greiner, J.; Haislip, J.; Kaper, L.; Knust, F.; Lacluyzé, A.; Milvang-Jensen, B.; Reichart, D.; Schulze, S.; Sudilovsky, V.; Tanvir, N. R.; Vergani, S. D.

doi:10.1093/mnras/stv960

Cited by 76 publications

(76 citation statements)

References 109 publications

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“…There are 40 published z > 0 quasar H 2 absorption systems (Levshakov & Varshalovich 1985;Ge & Bechtold 1997;Ge et al 2001;Ledoux et al 2002;Levshakov et al 2002;Reimers et al 2003;Ledoux et al 2003;Cui et al 2005;Ledoux et al 2006;Petitjean et al 2006;Noterdaeme et al 2007Noterdaeme et al , 2008Srianand et al 2008b;Jorgenson et al 2009;Malec et al 2009;Noterdaeme et al 2010;Jorgenson et al 2010;Fynbo et al 2011;Guimarães et al 2012;Srianand et al 2012;Crighton et al 2013;Oliveira et al 2014;Balashev et al 2015;Noterdaeme et al 2015b;Muzahid et al 2015Muzahid et al , 2016Krogager et al 2016;Noterdaeme et al 2017) and this paper. Also there are four H 2 -bearing systems detected in GRB afterglows Krühler et al 2013;Friis et al 2015;D'Elia et al 2014). As observed by several authors (e.g.…”

Section: Metallicity and Depletion Patternmentioning

confidence: 74%

CO-dark molecular gas at high redshift: very large H2 content and high pressure in a low-metallicity damped Lyman alpha system

Balashev

Noterdaeme

Rahmani

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of an H 2 -rich, extremely strong intervening damped Ly-α absorption system (DLA) at z abs = 2.786 towards the quasar J 0843+0221, observed with the Ultraviolet and Visual Echelle Spectrograph on the Very Large Telescope. The total column density of molecular (resp. atomic) hydrogen is log N(H 2 )=21.21 ± 0.02 (resp. log N(H i)=21.82 ± 0.11), making it to be the first case in quasar absorption line studies with H 2 column density as high as what is seen in 13 CO-selected clouds in the Milky-Way.We find that this system has one of the lowest metallicity detected among H 2 -bearing DLAs, with [Zn/H] = −1.52 +0.08 −0.10 . This can be the reason for the marked differences compared to systems with similar H 2 column densities in the local Universe: (i) the kinetic temperature, T ∼120 K, derived from the J = 0, 1 H 2 rotational levels is at least twice higher than expected; (ii) there is little dust extinction with A V < 0.1; (iii) no CO molecules are detected, putting a constraint on the X CO factor X CO > 2 × 10 23 cm −2 /(km/s K), in the very low metallicity gas. Low CO and high H 2 contents indicate that this system represents "CO-dark/faint" gas.We investigate the physical conditions in the H 2 -bearing gas using the fine-structure levels of C i, C ii, Si ii and the rotational levels of HD and H 2 . We find the number density to be about n ∼ 260 − 380 cm −3 , implying a high thermal pressure of 3 − 5 × 10 4 cm −3 K. We further identify a trend of increasing pressure with increasing total hydrogen column density. This independently supports the suggestion that extremely strong DLAs (with log N(H) ∼ 22) probe high-z galaxies at low impact parameters.

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Section: Metallicity and Depletion Patternmentioning

confidence: 74%

CO-dark molecular gas at high redshift: very large H2 content and high pressure in a low-metallicity damped Lyman alpha system

Balashev

Noterdaeme

Rahmani

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Indeed, Krühler et al (2011) find examples of heavily extinguished bursts in otherwise blue, low mass galaxies, as might be expected given this model. Friis et al (2015) and Heintz et al (2017) also find evidence for local dust properties which differ from the galaxy wide average. Furthermore, as figure 3 demonstrates, there is considerable overlap in absolute magnitudes between dark and bright GRB hosts.…”

Section: Host Galaxy -Grb Offsetsmentioning

confidence: 86%

Chandra and Hubble Space Telescope observations of dark gamma-ray bursts and their host galaxies

Chrimes

Levan

Stanway

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a study of 21 dark gamma-ray burst (GRB) host galaxies, predominantly using X-ray afterglows obtained with the Chandra X-Ray Observatory (CXO) to precisely locate the burst in deep Hubble Space Telescope (HST) imaging of the burst region. The host galaxies are well-detected in F160W in all but one case and in F606W imaging in ∼ 60 per cent of cases. We measure magnitudes and perform a morphological analysis of each galaxy. The asymmetry, concentration and ellipticity of the dark burst hosts are compared against the host galaxies of optically bright GRBs. In agreement with other studies, we find that dark GRB hosts are redder and more luminous than the bulk of the GRB host population. The distribution of projected spatial offsets for dark GRBs from their host galaxy centroids is comparable to that of optically-bright bursts. The dark GRB hosts are physically larger, more massive and redder, but are morphologically similar to the hosts of bright GRBs in terms of concentration and asymmetry. Our analysis constrains the fraction of high redshift (z > 5) GRBs in the sample to ∼14 per cent, implying an upper limit for the whole long-GRB population of ≤4.4 per cent. If dust is the primary cause of afterglow darkening amongst dark GRBs, the measured extinction may require a clumpy dust component in order to explain the observed offset and ellipticity distributions.

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“…Detailed spectroscopic observation of GRB hosts, however, remained challenging, in particular at z > 1: prominent tracers of the physical conditions in the hot gas are redshifted into the NIR where spectroscopy traditionally is much less efficient. Spectroscopic data for z > 1 GRB hosts from emission lines is therefore available for only a handful of cases (e.g., Chen 2012;Friis et al 2015;Piranomonte et al 2015), and even at z < 1 the largest samples (Savaglio et al 2009;Levesque et al 2010a;Graham & Fruchter 2013) contain only 10-15 events with detailed information on the host's gas properties.…”

Section: Introductionmentioning

confidence: 99%

GRB hosts through cosmic time

Krühler

Malesani

Fynbo

et al. 2015

A&A

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275

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We present data and initial results from VLT/X-Shooter emission-line spectroscopy of 96 galaxies selected by long γ-ray bursts (GRBs) at 0.1 < z < 3.6, the largest sample of GRB host spectra available to date. Most of our GRBs were detected by Swift and 76% are at 0.5 < z < 2.5 with a median z med ∼ 1.6. Based on Balmer and/or forbidden lines of oxygen, nitrogen, and neon, we measure systemic redshifts, star formation rates (SFR), visual attenuations (A V ), oxygen abundances (12 + log(O/H)), and emission-line widths (σ). We study GRB hosts up to z ∼ 3.5 and find a strong change in their typical physical properties with redshift. The median SFR of our GRB hosts increases from SFR med ∼ 0.6 M yr −1 atO ] at higher redshifts leads to an increasing distance of GRB-selected galaxies to the locus of local galaxies in the Baldwin-Phillips-Terlevich diagram. There is weak evidence for a redshift evolution in A V and σ, with the highest values seen at z ∼ 1.5 (A V ) or z ∼ 2 (σ). Oxygen abundances of the galaxies are distributed between 12 + log(O/H) = 7.9 and 12 + log(O/H) = 9.0 with a median 12 + log(O/H) med ∼ 8.5. The fraction of GRB-selected galaxies with super-solar metallicities is ∼20% at z < 1 in the adopted metallicity scale. This is significantly less than the fraction of total star formation in similar galaxies, illustrating that GRBs are scarce in high metallicity environments. At z ∼ 3, sensitivity limits us to probing only the most luminous GRB hosts for which we derive metallicities of Z 0.5 Z . Together with a high incidence of Z ∼ 0.5 Z galaxies at z ∼ 1.5, this indicates that a metallicity dependence at low redshift will not be dominant at z ∼ 3. Significant correlations exist between the hosts' physical properties. Oxygen abundance, for example, relates to A V (12 + log(O/H) ∝ 0.17 · A V ), line width (12 + log(O/H) ∝ σ 0.6 ), and SFR (12 + log(O/H) ∝ SFR 0.2 ). In the last two cases, the normalization of the relations shift to lower metallicities at z > 2 by ∼0.4 dex. These properties of GRB hosts and their evolution with redshift can be understood in a cosmological context of star-forming galaxies and a picture in which the hosts' properties at low redshift are influenced by the tendency of GRBs to avoid the most metal-rich environments.

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The warm, the excited, and the molecular gas: GRB 121024A shining through its star-forming galaxy★

Cited by 76 publications

References 109 publications

CO-dark molecular gas at high redshift: very large H2 content and high pressure in a low-metallicity damped Lyman alpha system

CO-dark molecular gas at high redshift: very large H2 content and high pressure in a low-metallicity damped Lyman alpha system

Chandra and Hubble Space Telescope observations of dark gamma-ray bursts and their host galaxies

GRB hosts through cosmic time

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