Probing dust-obscured star formation in the most massive gamma-ray burst host galaxies

Greiner, J.; Michalowski, Michal; Klose, S.; Hunt, L. K.; Gentile, Gianfranco; Kamphuis, P.; Herrero-Illana, R.; Wieringa, M.; Krühler, T.; Schady, P.; Elliott, J.; Graham, John F.; Ibar, E.; Knust, F.; Guelbenzu, A. Nicuesa; Palazzi, E.; Rossi, A.; Savaglio, S.

doi:10.1051/0004-6361/201628861

Cited by 35 publications

(51 citation statements)

References 77 publications

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“…The obtained upper limit is SFR < 30 M ⊙ yr −1 . In combination with earlier radio flux measurements of the afterglow, Greiner et al (2016) suggested that the radio emission reported in Stanway et al (2014) was due to the afterglow.…”

Section: Grb 100621amentioning

confidence: 61%

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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

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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.

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Section: Grb 100621amentioning

confidence: 61%

“…The SFR is 20-40 M ⊙ yr −1 based on the Hα line (Elliott et al 2013;Krühler et al 2015) and 66 M ⊙ yr −1 based on SED fitting (Elliott et al 2013). Radio 2.1 GHz observations by Greiner et al (2016) put an upper limit of SFR < 84 M ⊙ yr −1 .…”

Section: Grb 110918amentioning

confidence: 99%

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

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“…In this paper we assume that the radio emission is dominated by star-forming activity. SFRs based on the radio emission are derived by using the equation of Murphy et al (2011) for 1.4-GHz flux densities, which is used in previous studies of LGRB host galaxies (e.g., Perley et al 2015;Greiner et al 2016). Greiner et al (2016) extrapolate flux densities from the rest-frame frequency to 1.4 GHz and provide the equation of radio-derived SFRs as…”

Section: Resultsmentioning

confidence: 99%

Obscured Star Formation in the Host Galaxies of Superluminous Supernovae

Hatsukade

Tominaga

Hayashi

et al. 2018

ApJ

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We present the results of 3 GHz radio continuum observations of the 8 host galaxies of superluminous supernovae (SLSNe) at 0.1 < z < 0.3 by using the Karl G. Jansky Very Large Array. Four host galaxies are detected significantly, and two of them are found to have high star-formation rates (SFRs > 20 M ⊙ yr −1 ) derived from radio emission, making them the most intensely star-forming host galaxies among SLSN host galaxies. We compare radio SFRs and optical SFRs, and find that three host galaxies have an excess in radio SFRs by a factor of >2, suggesting the existence of dustobscured star formation, which cannot be traced by optical studies. Two of the three host galaxies, which are located in the galaxy main sequence based on optical SFRs, are found to be above the main sequence based on their radio SFRs. This suggests a higher fraction of starburst galaxies in SLSN hosts than estimated in previous studies. We calculate extinction from the ratio between radio SFRs and dust-uncorrected optical SFRs and find that the hosts are on the trend of increasing extinction with metallicity, which is consistent with the relation in local star-forming galaxies. We also place a constraint on a pulsar-driven SN model, which predicts quasi-steady synchrotron radio emission.

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“…The inset shows the 16th, 50th, and 84th percentiles of the marginalized star formation history, as well as the time-averaged SFR over the past 100 Myr, corresponding to the timescale of radio emission due to star formation. Right: Radio versus optical SFRs for PTF10hgi (green star), FRB121102 (purple star; assuming a star formation origin for the radio emission; Bassa et al 2017), LGRB hosts (yellow; Perley & Perley 2013;Perley et al 2015;Greiner et al 2016), and SLSN hosts (cyan; Hatsukade et al 2018). Upper limits are shown as open triangles.…”

Section: Origin Of the Radio Emissionmentioning

confidence: 99%

A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?

Eftekhari

Berger

Margalit

et al. 2019

ApJL

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We present the detection of an unresolved radio source coincident with the position of the Type I superluminous supernova (SLSN) PTF10hgi (z = 0.098) about 7.5 years post-explosion, with a luminosity of L ν (6 GHz) ≈ 1.1 × 10 28 erg s −1 Hz −1 . This represents the first detection of radio emission coincident with a SLSN on any timescale. We investigate various scenarios for the origin of the radio emission: star formation activity, an active galactic nucleus, an off-axis jet, and a non-relativistic supernova blastwave. While any of these would be quite novel if confirmed, none appear likely when taken in context of the other properties of the host galaxy, previous radio observations of SLSNe, the sample of long gamma-ray bursts (LGRBs), and the general population of hydrogen-poor SNe. Instead, the radio emission is reminiscent of the quiescent radio source associated with the repeating FRB121102, which has been argued to be powered by a magnetar born in a SLSN or LGRB explosion several decades ago. We show that such a central engine powered nebula is consistent with the age and luminosity of the radio source. Our directed search for FRBs from the location of PTF10hgi using 40 min of VLA phased-array data reveals no detections to a limit of 22 mJy (7σ; 10 ms duration). We outline several follow-up observations that can conclusively establish the origin of the radio emission.

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Probing dust-obscured star formation in the most massive gamma-ray burst host galaxies

Cited by 35 publications

References 77 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

Obscured Star Formation in the Host Galaxies of Superluminous Supernovae

A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?

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