A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION

Perley, D.; Levan, A. J.; Tanvir, N. R.; Cenko, S. Bradley; Bloom, J.; Hjorth, J.; Krühler, T.; Filippenko, A. V.; Fruchter, A. S.; Fynbo, J. P. U.; Jakobsson, P.; Kalirai, Jason; Milvang-Jensen, B.; Morgan, A. N.; Prochaska, J. Xavier; Silverman, J.

doi:10.1088/0004-637x/778/2/128

Cited by 183 publications

(277 citation statements)

References 203 publications

(317 reference statements)

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“…Such a sample is provided in Bloom et al (2002) but we find that for a number of the OTs in that sample better astrometry was subsequently provided by Fruchter et al (2006), and for those we reassess the impact parameters based on the Fruchter et al (2006) data. From the sample of Perley et al (2013) we include all GRBs for which coordinates of both hosts and OTs are provided with uncertainty 0.3 ′′ , and for which redshifts are known. The final values of impact parameters are presented in Table 5 and shown in histogram form in Fig 5. Based on this table we find that the mean, the weighted mean, and the median values are 2.3 kpc, 2.5 kpc, and 2.3 kpc respectively.…”

Section: Metallicity Gradientmentioning

confidence: 99%

“…The third and fourth columns present the impact parameter and corresponding error. a References: (1) Castro et al (2003); (2) Thöne et al (2013); (3) this work; (4) Bloom et al (2002); (5) Perley et al (2013) for the observed half galaxy. One could make the simple assumption that the cold clumps in the ISM and halo gas move randomly, but that most are bound inside the gravitational well.…”

Section: Potential Well Depthmentioning

confidence: 99%

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On the mass–metallicity relation, velocity dispersion, and gravitational well depth of GRB host galaxies

Arabsalmani

Møller

Fynbo

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We analyze a sample of 16 absorption systems intrinsic to long duration GRB host galaxies at z 2 for which the metallicities are known. We compare the relation between the metallicity and cold gas velocity width for this sample to that of the QSO-DLAs, and find complete agreement. We then compare the redshift evolution of the mass-metallicity relation of our sample to that of QSO-DLAs and find that also GRB hosts favour a late onset of this evolution, around a redshift of ≈ 2.6. We compute predicted stellar masses for the GRB host galaxies using the prescription determined from QSO-DLA samples and compare the measured stellar masses for the four hosts where stellar masses have been determined from SED fits. We find excellent agreement and conclude that, on basis of all available data and tests, long duration GRB-DLA hosts and intervening QSO-DLAs are consistent with being drawn from the same underlying population.GRB host galaxies and QSO-DLAs are found to have different impact parameter distributions and we briefly discuss how this may affect statistical samples. The impact parameter distribution has two effects. First any metallicity gradient will shift the measured metallicity away from the metallicity in the centre of the galaxy, second the path of the sightline through different parts of the potential well of the dark matter halo will cause different velocity fields to be sampled. We report evidence suggesting that this second effect may have been detected.

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Section: Metallicity Gradientmentioning

confidence: 99%

Section: Potential Well Depthmentioning

confidence: 99%

On the mass–metallicity relation, velocity dispersion, and gravitational well depth of GRB host galaxies

Arabsalmani

Møller

Fynbo

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…LGRB hosts at z < 1 are also found to be fainter and of lower stellar mass than a field star-forming galaxy population (see also Vergani et al 2015;Perley et al 2013Perley et al , 2016b. Because the stellar mass and metallicity of star-forming galaxies are correlated (stellar massmetallicity relation, Tremonti et al 2004), the low-metallicity preference could provide the explanation for the differences in observed stellar masses between populations.…”

Section: Introductionmentioning

confidence: 98%

“…Studies in the past have reached contradictory conclusions regarding the LGRB efficiency, largely because of the heterogeneous nature of investigated samples (e.g. Le Floc'h et al 2003Floc'h et al , 2006Fruchter et al 2006;Savaglio et al 2009;Levesque et al 2010a;Svensson et al 2010;Mannucci et al 2011;Graham & Fruchter 2013;Perley et al 2013;Hunt et al 2014). However, the large number of LGRBs detected by the Swift satellite (Gehrels et al 2004) accumulated in the past ten years and carefully chosen selection criteria have recently resulted in several unbiased LGRB samples, highly complete in redshift: the GROND , BAT6 , TOUGH , and SHOALS (Perley et al 2016a) samples.…”

Section: Introductionmentioning

confidence: 99%

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Japelj

Vergani

Salvaterra

et al. 2016

A&A

Self Cite

100

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Aims. Long gamma-ray bursts (LGRBs) are associated with the deaths of massive stars and might therefore be a potentially powerful tool for tracing cosmic star formation. However, especially at low redshifts (z < 1.5) LGRBs seem to prefer particular types of environment. Our aim is to study the host galaxies of a complete sample of bright LGRBs to investigate the effect of the environment on GRB formation. Methods. We studied host galaxy spectra of the Swift/BAT6 complete sample of 14 z < 1 bright LGRBs. We used the detected nebular emission lines to measure the dust extinction, star formation rate (SFR), and nebular metallicity (Z) of the hosts and supplemented the data set with previously measured stellar masses M . The distributions of the obtained properties and their interrelations (e.g. mass-metallicity and SFR-M relations) are compared to samples of field star-forming galaxies. Results. We find that LGRB hosts at z < 1 have on average lower SFRs than if they were direct star formation tracers. By directly comparing metallicity distributions of LGRB hosts and star-forming galaxies, we find a good match between the two populations up to 12 + log O H ∼ 8.4−8.5, after which the paucity of metal-rich LGRB hosts becomes apparent. The LGRB host galaxies of our complete sample are consistent with the mass-metallicity relation at similar mean redshift and stellar masses. The cutoff against high metallicities (and high masses) can explain the low SFR values of LGRB hosts. We find a hint of an increased incidence of starburst galaxies in the Swift/BAT6 z < 1 sample with respect to that of a field star-forming population. Given that the SFRs are low on average, the latter is ascribed to low stellar masses. Nevertheless, the limits on the completeness and metallicity availability of current surveys, coupled with the limited number of LGRB host galaxies, prevents us from investigating more quantitatively whether the starburst incidence is such as expected after taking into account the high-metallicity aversion of LGRB host galaxies.

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“…However, these host galaxy studies were optically biased, which when accounted for, systematically more massive galaxies were found (e.g., Krühler et al 2011;Rossi et al 2012). Despite this increase in more massive galaxies, there still existed a deficit of massive, metal-rich host galaxies (e.g., Graham & Fruchter 2013;Perley et al 2013), which lead to the strict metallicity cut-off being increased to Z < 0.5 Z .…”

Section: Manymentioning

confidence: 99%

The First Billion Years project: gamma-ray bursts at z > 5

Elliott

Khochfar

Greiner

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Long gamma-ray burst's (LGRB's) association to the death of massive stars suggest they could be used to probe the cosmic star formation history (CSFH) with high accuracy, due to their high luminosities. We utilise cosmological simulations from the First Billion Years project to investigate the biases between the CSFH and the LGRB rate at z > 5, assuming various different models and constraints on the progenitors of LGRBs. We populate LGRBs using a selection based on environmental properties and demonstrate that the LGRB rate should trace the CSFH to high redshifts. The measured LGRB rate suggests that LGRBs have opening angles of θ jet = 0.1 • , although the degeneracy with the progenitor model cannot rule out an underlying bias. We demonstrate that proxies that relate the LGRB rate with global LGRB host properties do not reflect the underlying LGRB environment, and are in fact a result of the host galaxy's spatial properties, such that LGRBs can exist in galaxies of solar metallicity. However, we find a class of host galaxies that have low stellar mass and are metal-rich, and that their metallicity dispersions would not allow low-metallicity environments. Detection of hosts with this set of properties would directly reflect the progenitor's environment. We predict that 10% of LGRBs per year are associated with this set of galaxies that would have forbidden line emission that could be detected by instruments on the James Webb Space Telescope. Such a discovery would place strong constraints on the collapsar model and suggest other avenues to be investigated.

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A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION

Cited by 183 publications

References 203 publications

On the mass–metallicity relation, velocity dispersion, and gravitational well depth of GRB host galaxies

On the mass–metallicity relation, velocity dispersion, and gravitational well depth of GRB host galaxies

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

The First Billion Years project: gamma-ray bursts at z > 5

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