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

Hatsukade, Bunyo; Ohta, Kouji; Hashimoto, Tetsuya; Kohno, Kotaro; Nakanishi, Koichiro; Niino, Yuu; Tamura, Motohide

doi:10.3847/1538-4357/ab7992

Cited by 12 publications

(9 citation statements)

References 158 publications

(281 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For the hosts of GRBs 120815A and 181020A, the upper limits are weaker than expected from their host stellar masses, whereas the limit on the molecular gas mass in GRB 080607 is close to that expected from its host stellar mass. Overall, most of the CO detections in GRB hosts do fall between the curves with M = 10 10 − 10 11 M (Hatsukade et al 2020), as expected from their stellar masses, though some hosts appear to show significant molecular deficits (in particular at z 1).…”

Section: Mass and Redshift Dependence Of α Cosupporting

confidence: 53%

“…GRB hosts (Hatsukade et al 2020) GRB hosts (upper limits) H2 GRB hosts ( CO (Z/Z ) 1.4 ) H2 GRB hosts ( CO = CO, MW) QSO-DLAs (Kanekar et al 2020) (Upper lim. )…”

Section: Resultsmentioning

confidence: 99%

“…−1 (Bolatto et al 2013). For comparison, we overplot the recent compilation of CO observations of GRB host galaxies from Hatsukade et al (2020), spanning the redshift range z = 0.0 − 2.5. In addition, we show the track that broadly characterizes the molecular gas mass evolution of M > 10 10 M mainsequence star-forming galaxies, M mol /M = 0.1 × (1 + z) 2 (Geach et al 2011;Carilli & Walter 2013).…”

Section: Resultsmentioning

confidence: 99%

“…This has been done extensively for GRB hosts at UV to optical wavelengths (e.g., Krühler et al 2015;Arabsalmani et al 2018a;Corre et al 2018). Similarly, surveys targeting GRB hosts at sub-mm wavelengths, in particular the molecular emission from carbon monoxide (CO) have advanced over the last few years (Kohno et al 2005;Endo et al 2007;Hatsukade et al 2007Hatsukade et al , 2011Hatsukade et al , 2014Hatsukade et al , 2019Hatsukade et al , 2020Stanway et al 2011Stanway et al , 2015Arabsalmani et al 2018b;Michałowski et al 2016Michałowski et al , 2018de Ugarte Postigo et al 2020), largely due to the commissioning of the Atacama Large Millimeter/submillimeter Array (ALMA). Until now, however, only blind surveys or individual detections of CO emission in GRB host galaxies have been carried out.…”

mentioning

confidence: 99%

See 3 more Smart Citations

GRB host galaxies with strong H$_2$ absorption: CO-dark molecular gas at the peak of cosmic star formation

Heintz,

Björnsson,

Neeleman

et al. 2021

Preprint

View full text Add to dashboard Cite

We present a pilot search of CO emission in three H 2 -absorbing, long-duration gamma-ray burst (GRB) host galaxies at z ∼ 2−3. We used the Atacama Large Millimeter/sub-millimeter Array (ALMA) to target the CO(3 − 2) emission line and report nondetections for all three hosts. These are used to place limits on the host molecular gas masses, assuming a metallicity-dependent CO-to-H 2 conversion factor (α CO ). We find, M mol < 3.5 × 10 10 M (GRB 080607), M mol < 4.7 × 10 11 M (GRB 120815A), and M mol < 8.9 × 10 11 M (GRB 181020A). The high limits on the molecular gas mass for the latter two cases are a consequence of their low stellar masses M (M 10 8 M ) and low gas-phase metallicities (Z ∼ 0.03 Z ). The limit on the M mol /M ratio derived for GRB 080607, however, is consistent with the average population of star-forming galaxies at similar redshifts and stellar masses. We discuss the broader implications for a metallicity-dependent CO-to-H 2 conversion factor, and demonstrate that the canonical Galactic α CO , will severely underestimate the actual molecular gas mass for all galaxies at z > 1 with M < 10 10 M . To better quantify this we develop a simple approach to estimate the relevant α CO factor based only on the redshift and stellar mass of individual galaxies. The elevated conversion factors will make these galaxies appear CO-"dark" and difficult to detect in emission, as is the case for the majority of GRB hosts. GRB spectroscopy thus offers a complementary approach to identify low-metallicity, star-forming galaxies with abundant molecular gas reservoirs at high redshifts that are otherwise missed by current ALMA surveys.

show abstract

Section: Mass and Redshift Dependence Of α Cosupporting

confidence: 53%

“…GRB hosts (Hatsukade et al 2020) GRB hosts (upper limits) H2 GRB hosts ( CO (Z/Z ) 1.4 ) H2 GRB hosts ( CO = CO, MW) QSO-DLAs (Kanekar et al 2020) (Upper lim. )…”

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

mentioning

confidence: 99%

See 2 more Smart Citations

GRB host galaxies with strong H$_2$ absorption: CO-dark molecular gas at the peak of cosmic star formation

Heintz,

Björnsson,

Neeleman

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…The central and NW regions are molecule rich for their star formation rates (SFRs), but the SE region turned out to be molecule deficient. The total molecular gas mass turned out to be similar to that of other galaxies with similar redshift, star SFR, and stellar mass (Michałowski et al 2018b;Hatsukade et al 2020). Michałowski et al (2015) examined the H I line in five GRB host galaxies at z < 0.12, including the GRB 111005A host, using archival H I line from the Nançay radio telescope (Theureau et al 1998;Springob et al 2005).…”

Section: Introductionmentioning

confidence: 92%

The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A

Leśniewska

Michałowski

Kamphuis

et al. 2022

ApJS

View full text Add to dashboard Cite

Long (>2 s) gamma-ray bursts (GRBs) are associated with explosions of massive stars, although in three instances, supernovae (SNe) have not been detected, despite deep observations. With new H i line and archival optical integral-field spectroscopy data, we characterize the interstellar medium (ISM) of the host galaxy of one of these events, GRB 111005A, in order to shed light on the unclear nature of these peculiar objects. We found that the atomic gas, radio continuum, and rotational patterns are in general very smooth throughout the galaxy, which does not indicate a recent gas inflow or outflow. There is also no gas concentration around the GRB position. The ISM in this galaxy differs from that in hosts of other GRBs and SNe, which may suggest that the progenitor of GRB 111005A was not an explosion of a very massive star (e.g., a compact object merger). However, there are subtle irregularities of the GRB 111005A host (most at a 2σ level), which may point to a weak gas inflow or interaction. Because in the SE part of the host there is 15% more atomic gas and half the molecular gas than in the NW part, the molecular gas fraction is low. In the SE part there is also a region with a very high Hα equivalent width. There is more continuum 1.4 GHz emission to the SE and an S-shaped warp in the UV. Finally, there is also a low-metallicity region 3.″5 (1 kpc) from the GRB position. Two galaxies within 300 kpc or a past merger can be responsible for these irregularities.

show abstract

The host of GRB 171205A in 3D

Thöne,

de Ugarte Postigo,

Izzo

et al. 2024

A&A

View full text Add to dashboard Cite

Long GRB hosts at $z<1$ are usually low-mass, low-metallicity star-forming galaxies. Here we present the most detailed, spatially resolved study of the host of GRB 171205A so far, a grand-design barred spiral galaxy at $z=0.036$. Our analysis includes MUSE integral field spectroscopy complemented with high-spatial-resolution UV/VIS HST imaging and CO(1--0) and H i 21cm data. The GRB is located in a small star-forming region in a spiral arm of the galaxy at a deprojected distance of sim 8\,kpc from the center. The galaxy shows a smooth negative metallicity gradient and the metallicity at the GRB site is half solar, slightly below the mean metallicity at the corresponding distance from the center. Star formation in this galaxy is concentrated in a few H ii regions between 5 and 7\,kpc from the center and at the end of the bar, inwards from the GRB region; however the H ii region hosting the GRB is in the top 10<!PCT!> of the regions with the highest specific star-formation rate. The stellar population at the GRB site has a very young component ($<$ 5\,Myr) that contributes a significant part of the light. Ionized and molecular gas show only minor deviations at the end of the bar. A parallel study found an asymmetric H i distribution and some additional gas near the position of the GRB, which might explain the star-forming region of the GRB site. Our study shows that long GRBs can occur in many types of star-forming galaxies; however the actual GRB sites have consistently low metallicity, high star formation rates, and a young population. Furthermore, gas inflow or interactions triggering the star formation producing the GRB progenitor might not be evident in ionized or even molecular gas but only in H i

show abstract

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

Cited by 12 publications

References 158 publications

GRB host galaxies with strong H$_2$ absorption: CO-dark molecular gas at the peak of cosmic star formation

GRB host galaxies with strong H$_2$ absorption: CO-dark molecular gas at the peak of cosmic star formation

The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A

The host of GRB 171205A in 3D

Contact Info

Product

Resources

About