Super-solar metallicity at the position of the ultra-long GRB 130925A

Schady, P.; Krühler, T.; Greiner, J.; Graham, John F.; Канн, Д. А.; Bolmer, J.; Delvaux, C.; Elliott, J.; Klose, S.; Knust, F.; Guelbenzu, A. Nicuesa; Rau, A. R. P.; Rossi, A.; Savaglio, S.; Schmidl, S.; Schweyer, T.; Sudilovsky, V.; Tanga, M.; Tanvir, N. R.; Varela, K.; Wiseman, P.

doi:10.1051/0004-6361/201526060

Cited by 38 publications

(42 citation statements)

References 94 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The afterglow spectrum shows a high visual extinction (A V = 5.0 ± 0.7 mag; Greiner et al 2014) that is one of the largest extinction among GRB afterglows. The host also shows a high extinction of A V = 2.4 ± 0.9 mag based on SED fitting (Schady et al 2015). Optical spectroscopy of the host shows two star-forming regions corresponding to the galaxy nucleus and an Hii region located ∼0.…”

Section: Grb 130925amentioning

confidence: 91%

“…Optical spectroscopy of the host shows two star-forming regions corresponding to the galaxy nucleus and an Hii region located ∼0. ′′ 2 (6 kpc in projection) southwest of the nucleus (Schady et al 2015). The GRB site is close to the nucleus, which has a super-solar metallicity (Schady et al 2015;Krühler et al 2015).…”

Section: Grb 130925amentioning

confidence: 99%

“…The GRB site is close to the nucleus, which has a super-solar metallicity (Schady et al 2015;Krühler et al 2015). The SFR in the host is 2-3 M ⊙ yr −1 based on the Hα line and SED fitting (Schady et al 2015;Krühler et al 2015).…”

Section: Grb 130925amentioning

confidence: 99%

See 2 more Smart Citations

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

Hatsukade

Ohta

Hashimoto

et al. 2020

ApJ

View full text Add to dashboard Cite

We present the results of CO observations toward 14 host galaxies of long-duration gamma-ray bursts (GRBs) at z = 0.1-2.5 by using the Atacama Large Millimeter/submillimeter Array. We successfully detected CO(3-2) or CO(4-3) emission in eight hosts (z = 0.3-2), which more than doubles the sample size of GRB hosts with CO detection. The derived molecular gas mass is M gas = (0.2-6) × 10 10 M ⊙ assuming metallicity-dependent CO-to-H 2 conversion factors. By using the largest sample of GRB hosts with molecular gas estimates (25 in total, of which 14 are CO-detected) including results from the literature, we compared molecular gas properties with those of other star-forming galaxies (SFGs). The GRB hosts tend to have a higher molecular gas mass fraction (µ gas ) and a shorter gas depletion timescale (t depl ) as compared with other SFGs at similar redshifts especially at z 1. This could be a common property of GRB hosts or an effect introduced by the selection of targets which are typically above the main-sequence line. To eliminate the effect of selection bias, we analyzed µ gas and t depl as a function of the distance from the main-sequence line (δMS). We find that the GRB hosts follow the same scaling relations as other SFGs, where µ gas increases and t depl decreases with increasing δMS. No molecular gas deficit is observed when compared to other SFGs of similar SFR and stellar mass. These findings suggest that the same star-formation mechanism is expected to be happening in GRB hosts as in other SFGs.

show abstract

Section: Grb 130925amentioning

confidence: 91%

Section: Grb 130925amentioning

confidence: 99%

See 1 more Smart Citation

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

Hatsukade

Ohta

Hashimoto

et al. 2020

ApJ

View full text Add to dashboard Cite

show abstract

“…However, this picture is complicated by the fact that some GRBs have been found in galaxies with solar or supersolar metallicities Levesque et al 2010b;Krühler et al 2012a;Savaglio et al 2012;Elliott et al 2013;Schulze et al 2014;Stanway et al 2015a;Hashimoto et al 2015;Schady et al 2015). This can be explained in two ways.…”

Section: H 2 Vs H I: What Is the Fuel Of Star Formation?mentioning

confidence: 99%

Massive stars formed in atomic hydrogen reservoirs: H I observations of gamma-ray burst host galaxies

Michałowski

Gentile

Hjorth

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

Long gamma-ray bursts (GRBs), among the most energetic events in the Universe, are explosions of massive and short-lived stars, so they pinpoint locations of recent star formation. However, several GRB host galaxies have recently been found to be deficient in molecular gas (H 2 ), believed to be the fuel of star formation. Moreover, optical spectroscopy of GRB afterglows implies that the molecular phase constitutes only a small fraction of the gas along the GRB line of sight. Here we report the first ever 21 cm line observations of GRB host galaxies, using the Australia Telescope Compact Array, implying high levels of atomic hydrogen (H i), which suggests that the connection between atomic gas and star formation is stronger than previously thought. In this case, it is possible that star formation is directly fuelled by atomic gas (or that the H i-to-H 2 conversion is very efficient, which rapidly exhaust molecular gas), as has been theoretically shown to be possible. This can happen in low-metallicity gas near the onset of star formation because cooling of gas (necessary for star formation) is faster than the H i-to-H 2 conversion. Indeed, large atomic gas reservoirs, together with low molecular gas masses, stellar, and dust masses are consistent with GRB hosts being preferentially galaxies which have very recently started a star formation episode after accreting metal-poor gas from the intergalactic medium. This provides a natural route for forming GRBs in low-metallicity environments. The gas inflow scenario is also consistent with the existence of the companion H i object with no optical counterpart ∼19 kpc from the GRB 060505 host, and with the fact that the H i centroids of the GRB 980425 and 060505 hosts do not coincide with optical centres of these galaxies, but are located close to the GRB positions.

show abstract

“…GRBs are not exclusively found at such low metallicity, with observed examples arising in environments exceeding Solar abundance (e.g. Graham et al 2009;Levesque et al 2010b;Schady et al 2015;Micha lowski et al 2018). QHE therefore cannot be the sole contributing pathway.…”

Section: Introductionmentioning

confidence: 99%

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Chrimes

Stanway

Eldridge

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Long-duration gamma-ray bursts (GRBs) are understood to be the final fate for a subset of massive, stripped envelope, rapidly rotating stars. Beyond this, our knowledge of the progenitor systems is limited. Using the BPASS (Binary Population and Spectral Synthesis) stellar evolution models, we investigate the possibility that some massive stars in binaries can maintain the angular momentum required for jet production, while still loosing their outer envelope through winds or binary interactions. We find that a total hydrogen mass of M H < 5 × 10 −4 M and a helium ejecta mass fraction of F He < 0.20 provide the best thresholds for the supernova II/Ibc and Ib/Ic divisions respectively. Tidal interactions in binaries are accounted for by applying a tidal algorithm to post-process the stellar evolution models output by BPASS. We show that the observed volumetric gamma-ray burst rate evolution can be recreated using two distinct pathways and plausible distributions for burst parameters. In the first pathway, stars are spun up by mass accretion into a quasi-homogeneous state. In the second, tides maintain rotation where otherwise the star would spin down. Both lead to type Ic supernova progenitors, and a metallicity distribution consistent with the GRB host galaxy population. The inferred core angular momentum threshold for jet production is consistent with theoretical requirements for collapsars, given the assumptions made in our model. We can therefore reproduce several aspects of core collapse supernova/GRB observation and theory simultaneously. We discuss the predicted observable properties of GRB progenitors and their surviving companions.

show abstract

Super-solar metallicity at the position of the ultra-long GRB 130925A

Cited by 38 publications

References 94 publications

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations

Massive stars formed in atomic hydrogen reservoirs: H I observations of gamma-ray burst host galaxies

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Contact Info

Product

Resources

About