Outflows from GRB hosts are ubiquitous: Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES

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Standard

Outflows from GRB hosts are ubiquitous : Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES. / Thoene, C. C.; Izzo, L.; Flores, H.; de Ugarte Postigo, A.; Vergani, S. D.; Agui Fernandez, J. F.; Kann, D. A.; Christensen, L.; Covino, S.; Della Valle, M.; Hammer, F.; Melandri, A.; Puech, M.; Rodrigues, M. A.; Gorosabel, J.

I: Astronomy & Astrophysics, Bind 656, A136, 15.12.2021.

Publikation: Bidrag til tidsskriftTidsskriftartikelForskningfagfællebedømt

Harvard

Thoene, CC, Izzo, L, Flores, H, de Ugarte Postigo, A, Vergani, SD, Agui Fernandez, JF, Kann, DA, Christensen, L, Covino, S, Della Valle, M, Hammer, F, Melandri, A, Puech, M, Rodrigues, MA & Gorosabel, J 2021, 'Outflows from GRB hosts are ubiquitous: Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES', Astronomy & Astrophysics, bind 656, A136. https://doi.org/10.1051/0004-6361/201935652

APA

Thoene, C. C., Izzo, L., Flores, H., de Ugarte Postigo, A., Vergani, S. D., Agui Fernandez, J. F., Kann, D. A., Christensen, L., Covino, S., Della Valle, M., Hammer, F., Melandri, A., Puech, M., Rodrigues, M. A., & Gorosabel, J. (2021). Outflows from GRB hosts are ubiquitous: Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES. Astronomy & Astrophysics, 656, [A136]. https://doi.org/10.1051/0004-6361/201935652

Vancouver

Thoene CC, Izzo L, Flores H, de Ugarte Postigo A, Vergani SD, Agui Fernandez JF o.a. Outflows from GRB hosts are ubiquitous: Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES. Astronomy & Astrophysics. 2021 dec. 15;656. A136. https://doi.org/10.1051/0004-6361/201935652

Author

Thoene, C. C. ; Izzo, L. ; Flores, H. ; de Ugarte Postigo, A. ; Vergani, S. D. ; Agui Fernandez, J. F. ; Kann, D. A. ; Christensen, L. ; Covino, S. ; Della Valle, M. ; Hammer, F. ; Melandri, A. ; Puech, M. ; Rodrigues, M. A. ; Gorosabel, J. / Outflows from GRB hosts are ubiquitous : Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES. I: Astronomy & Astrophysics. 2021 ; Bind 656.

Bibtex

@article{071cfb038d254ed0b1e82dab7da99d69,
title = "Outflows from GRB hosts are ubiquitous: Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES",
abstract = "The hosts of long duration gamma-ray bursts (GRBs) are predominantly starburst galaxies at subsolar metallicity. At redshifts z < 1, this implies that most of them are low-mass galaxies similar to the populations of blue compact dwarfs and dwarf irregulars. What triggers the massive star-formation needed for producing a GRB progenitor is still largely unknown, as are the resolved gas properties and kinematics of these galaxies and their formation history. Here we present a sample of six spatially resolved GRB hosts at z < 0:3 observed with 3D spectroscopy at high spectral resolution (R = 8000-13 000) using FLAMES /VLT. We analyzed the resolved gas kinematics of the full sample and the abundances in a subsample with strong enough emission lines. Only two galaxies show a regular disk-like rotation field, another two are dispersion-dominated, and the remaining ones have two narrow emission components associated with di fferent parts of the galaxy but no regular rotation field, which might indicate a recent merger. All galaxies show evidence for broad components underlying the main emission peak with sigma of 50 110 km s(-1). This broad component is more metalrich than the narrow components, it is blueshifted in most cases, and it follows a di fferent velocity structure. We find a weak correlation between the star-formation rate and the width of the broad component, its flux compared to the narrow component, and the maximum outflow velocity of the gas, but we do not find any correlation with the star-formation density, metallicity or stellar mass. We hence associate this broad component with a metal-rich outflow from star-forming regions in the host. The GRB is not located in the brightest region of the host, but is always associated with some star-forming region showing a clear wind component. Our study shows the great potential of 3D spectroscopy to study the star-formation processes and history in galaxies hosting extreme transients, the need for high signal-to-noise, and the perils using unresolved or only partially resolved data for these kinds of studies.",
keywords = "gamma-ray burst: general, galaxies: starburst, galaxies: kinematics and dynamics, GAMMA-RAY BURST, CORE-COLLAPSE SUPERNOVAE, COMPACT DWARF GALAXIES, SPACE-TELESCOPE OBSERVATIONS, INTEGRAL FIELD SPECTROSCOPY, MASS-METALLICITY RELATION, STAR-FORMING GALAXIES, EMISSION-LINE RATIOS, METAL-POOR GALAXIES, H II REGION",
author = "Thoene, {C. C.} and L. Izzo and H. Flores and {de Ugarte Postigo}, A. and Vergani, {S. D.} and {Agui Fernandez}, {J. F.} and Kann, {D. A.} and L. Christensen and S. Covino and {Della Valle}, M. and F. Hammer and A. Melandri and M. Puech and Rodrigues, {M. A.} and J. Gorosabel",
year = "2021",
month = dec,
day = "15",
doi = "10.1051/0004-6361/201935652",
language = "English",
volume = "656",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - Outflows from GRB hosts are ubiquitous

T2 - Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES

AU - Thoene, C. C.

AU - Izzo, L.

AU - Flores, H.

AU - de Ugarte Postigo, A.

AU - Vergani, S. D.

AU - Agui Fernandez, J. F.

AU - Kann, D. A.

AU - Christensen, L.

AU - Covino, S.

AU - Della Valle, M.

AU - Hammer, F.

AU - Melandri, A.

AU - Puech, M.

AU - Rodrigues, M. A.

AU - Gorosabel, J.

PY - 2021/12/15

Y1 - 2021/12/15

N2 - The hosts of long duration gamma-ray bursts (GRBs) are predominantly starburst galaxies at subsolar metallicity. At redshifts z < 1, this implies that most of them are low-mass galaxies similar to the populations of blue compact dwarfs and dwarf irregulars. What triggers the massive star-formation needed for producing a GRB progenitor is still largely unknown, as are the resolved gas properties and kinematics of these galaxies and their formation history. Here we present a sample of six spatially resolved GRB hosts at z < 0:3 observed with 3D spectroscopy at high spectral resolution (R = 8000-13 000) using FLAMES /VLT. We analyzed the resolved gas kinematics of the full sample and the abundances in a subsample with strong enough emission lines. Only two galaxies show a regular disk-like rotation field, another two are dispersion-dominated, and the remaining ones have two narrow emission components associated with di fferent parts of the galaxy but no regular rotation field, which might indicate a recent merger. All galaxies show evidence for broad components underlying the main emission peak with sigma of 50 110 km s(-1). This broad component is more metalrich than the narrow components, it is blueshifted in most cases, and it follows a di fferent velocity structure. We find a weak correlation between the star-formation rate and the width of the broad component, its flux compared to the narrow component, and the maximum outflow velocity of the gas, but we do not find any correlation with the star-formation density, metallicity or stellar mass. We hence associate this broad component with a metal-rich outflow from star-forming regions in the host. The GRB is not located in the brightest region of the host, but is always associated with some star-forming region showing a clear wind component. Our study shows the great potential of 3D spectroscopy to study the star-formation processes and history in galaxies hosting extreme transients, the need for high signal-to-noise, and the perils using unresolved or only partially resolved data for these kinds of studies.

AB - The hosts of long duration gamma-ray bursts (GRBs) are predominantly starburst galaxies at subsolar metallicity. At redshifts z < 1, this implies that most of them are low-mass galaxies similar to the populations of blue compact dwarfs and dwarf irregulars. What triggers the massive star-formation needed for producing a GRB progenitor is still largely unknown, as are the resolved gas properties and kinematics of these galaxies and their formation history. Here we present a sample of six spatially resolved GRB hosts at z < 0:3 observed with 3D spectroscopy at high spectral resolution (R = 8000-13 000) using FLAMES /VLT. We analyzed the resolved gas kinematics of the full sample and the abundances in a subsample with strong enough emission lines. Only two galaxies show a regular disk-like rotation field, another two are dispersion-dominated, and the remaining ones have two narrow emission components associated with di fferent parts of the galaxy but no regular rotation field, which might indicate a recent merger. All galaxies show evidence for broad components underlying the main emission peak with sigma of 50 110 km s(-1). This broad component is more metalrich than the narrow components, it is blueshifted in most cases, and it follows a di fferent velocity structure. We find a weak correlation between the star-formation rate and the width of the broad component, its flux compared to the narrow component, and the maximum outflow velocity of the gas, but we do not find any correlation with the star-formation density, metallicity or stellar mass. We hence associate this broad component with a metal-rich outflow from star-forming regions in the host. The GRB is not located in the brightest region of the host, but is always associated with some star-forming region showing a clear wind component. Our study shows the great potential of 3D spectroscopy to study the star-formation processes and history in galaxies hosting extreme transients, the need for high signal-to-noise, and the perils using unresolved or only partially resolved data for these kinds of studies.

KW - gamma-ray burst: general

KW - galaxies: starburst

KW - galaxies: kinematics and dynamics

KW - GAMMA-RAY BURST

KW - CORE-COLLAPSE SUPERNOVAE

KW - COMPACT DWARF GALAXIES

KW - SPACE-TELESCOPE OBSERVATIONS

KW - INTEGRAL FIELD SPECTROSCOPY

KW - MASS-METALLICITY RELATION

KW - STAR-FORMING GALAXIES

KW - EMISSION-LINE RATIOS

KW - METAL-POOR GALAXIES

KW - H II REGION

U2 - 10.1051/0004-6361/201935652

DO - 10.1051/0004-6361/201935652

M3 - Journal article

VL - 656

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A136

ER -

ID: 288787479