“DARK” GRB 080325 IN A DUSTY MASSIVE GALAXY AT<i>z</i>∼ 2

Hashimoto, Tetsuya; Ohta, Kouji; Aoki, Kentaro; Tanaka, Ichi; Yabe, Kiyoto; Kawai, N.; Aoki, Wako; Furusawa, Hisanori; Hattori, Takashi; Iye, Masanori; Kawabata, Koji S.; Kobayashi, Naoto; Komiyama, Yutaka; Kosugi, George; Minowa, Yosuke; Mizumoto, Y.; Niino, Yuu; Nomoto, Ken’ichi; Noumaru, Junichi; Ogasawara, Ryusuke; Pyo, Tae‐Soo; Sakamoto, T.; Sekiguchi, K.; Shirasaki, Y.; Suzuki, M.; Tajitsu, Akito; Takata, Tadafumi; Tamagawa, Toru; Terada, Hiroshi; Totani, Tomonori; Watanabe, Jun; Yamada, Tōru; Yoshida, A.

doi:10.1088/0004-637x/719/1/378

Cited by 28 publications

(39 citation statements)

References 53 publications

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“…The observed broad-band SED is indicative of a very luminous (M K ∼ 24.4), infrared-bright galaxy, very different from the sample of GRBHs compiled by SBG09. This host galaxy is similar in color, luminosity, and redshift to the hosts of the dark bursts GRB 020127 ), GRB 030115 , and GRB 080325 (Hashimoto et al 2010). There is possibly a bias in the GRB host samples studied so far, which are dominated by host galaxies of optically detected afterglows.…”

Section: Eros As An Important Subpopulation Of Grb Host Galaxiesmentioning

confidence: 70%

“…While many of these non-detections are simply due to the lack of rapid and deep optical follow-up observations, some events (after correction for Galactic extinction) are truly optically dark (e.g., Fynbo et al 2001;De Pasquale et al 2003;Castro-Tirado et al 2007;Rol et al 2007;Hashimoto et al 2010;Holland et al 2010).…”

Section: Bursts With Optically Undetected Afterglowsmentioning

confidence: 99%

“…Among them, the most extreme cases are classified as EROs. To date, only a small number of GRB hosts have been found that enter this category: GRB 020127 ), GRB 030115 Dullighan et al 2004), GRB 080207 (Hunt et al 2011;Svensson et al 2012), as well as GRB 080325 (Hashimoto et al 2010). …”

Section: Extremely Red Objects As Candidatesmentioning

confidence: 99%

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A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

Rossi

Klose

Ferrero

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) can provide information about star formation at high redshifts. Even in the absence of a bright optical/nearinfrared/radio afterglow, the high detection rate of X-ray afterglows by Swift/XRT and its localization precision of 2-3 arcsec facilitates the identification and the study of GRB host galaxies. Aims. We focus on the search for the host galaxies of 17 bursts with arcsec-sized XRT error circles but no detected long-wavelength afterglow, in spite of their deep and rapid follow-up observations. Three of these events can also be classified as truly dark bursts, i.e., the observed upper limit on the optical flux of the afterglow was less than expected based on the measured X-ray flux. Our goals are to identify the GRB host galaxy candidates and characterize their phenomenological parameters. Methods. Our study is based on deep R C and K s -band observations performed with FORS1, FORS2, VIMOS, ISAAC, and HAWK-I at the ESO/VLT, partly supported by observations with the seven-channel imager GROND at the 2.2-m telescope on La Silla, and supplemented by observations with NEWFIRM at the 4-m telescope on Kitt Peak. To be conservative, we searched for host galaxy candidates within an area of twice the radius of each associated 90% c.l. Swift/XRT error circle. Results. For 15 of the 17 bursts, we find at least one galaxy within the searching area, and in the remaining two cases only a deep upper limit to R C and K s can be provided. In seven cases, we discover extremely red objects in the error circles, at least four of which might be dust-enshrouded galaxies. The most remarkable case is the host of GRB 080207, which has a color of (R C − K s ) AB ∼ 4.7 mag, and is one of the reddest galaxies ever associated with a GRB. As a by-product of our study we identify the optical afterglow of GRB 070517. Conclusions. Only a minority of optically dim afterglows are due to Lyman dropout ( 1/3). Extinction by dust in the host galaxies might explain all other events. Thereby, a seemingly non-negligible fraction of these hosts are globally dust-enshrouded, extremely red galaxies. This suggests that at least a fraction of GRB afterglows trace a subpopulation of massive starburst galaxies, which are markedly different from the main body of the GRB host galaxy population, namely the blue, subluminous, compact galaxies.

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Section: Eros As An Important Subpopulation Of Grb Host Galaxiesmentioning

confidence: 70%

Section: Bursts With Optically Undetected Afterglowsmentioning

confidence: 99%

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A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

Rossi

Klose

Ferrero

et al. 2012

A&A

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“…Previous sample studies (e.g., Berger et al 2003;Le Floc'h et al 2003;Perley et al 2009) have not revealed strong evidence of a strong diversity. A handful of single dark GRBs have however been found to be hosted by red and dusty galaxies with high metallicities and stellar masses over 10 11 M (e.g., Levan et al 2006;Berger et al 2007; Levesque et al 2010;Hashimoto et al 2010;Küpcü Yoldaş et al 2010;Chen et al 2010). Recently Perley et al (2010aPerley et al ( , 2011a indicate that the general galaxy population hosting dark bursts is redder and more luminous than those selected via optically bright afterglows.…”

Section: Introductionmentioning

confidence: 99%

The SEDs and host galaxies of the dustiest GRB afterglows

Krühler

Greiner

Schady

et al. 2011

A&A

170

271

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Context. The afterglows and host galaxies of long gamma-ray bursts (GRBs) offer unique opportunities to study star-forming galaxies in the high-z Universe. Until recently, however, the information inferred from GRB follow-up observations was mostly limited to optically bright afterglows, biasing all demographic studies against sight-lines that contain large amounts of dust. Aims. Here we present afterglow and host observations for a sample of bursts that are exemplary of previously missed ones because of high visual extinction (A GRB V 1 mag) along the sight-line. This facilitates an investigation of the properties, geometry, and location of the absorbing dust of these poorly-explored host galaxies, and a comparison to hosts from optically-selected samples. Methods. This work is based on GROND optical/NIR and Swift/XRT X-ray observations of the afterglows, and multi-color imaging for eight GRB hosts. The afterglow and galaxy spectral energy distributions yield detailed insight into physical properties such as the dust and metal content along the GRB sight-line and galaxy-integrated characteristics such as the host's stellar mass, luminosity, color-excess, and star-formation rate. Results. For the eight afterglows considered in this study, we report for the first time the redshift of GRB 081109 (z = 0.9787±0.0005), and the visual extinction towards GRBs 081109 (A GRB V = 3.4 +0.4 −0.3 mag) and 100621A (A GRB V = 3.8 ± 0.2 mag), which are among the largest ever derived for GRB afterglows. Combined with non-extinguished GRBs, there is a strong anti-correlation between the afterglow's metal-to-dust ratio and visual extinction. The hosts of the dustiest afterglows are diverse in their properties, but on average redder ( (R − K) AB ∼ 1.6 mag), more luminous ( L ∼ 0.9 L * ), and massive ( log M * [M ] ∼ 9.8) than the hosts of optically-bright events. Hence, we probe a different galaxy population, suggesting that previous host samples miss most of the massive and metal-rich members. This also indicates that the dust along the sight-line is often related to host properties, and thus probably located in the diffuse ISM or interstellar clouds and not in the immediate GRB environment. Some of the hosts in our sample, are blue, young, or of low stellar mass illustrating that even apparently non-extinguished galaxies possess very dusty sight-lines owing to a patchy dust distribution. Conclusions. The afterglows and host galaxies of the dustiest GRBs provide evidence of a complex dust geometry in star-forming galaxies. In addition, they establish a population of luminous, massive, and correspondingly chemically evolved GRB hosts. This suggests that GRBs trace the global star-formation rate better than studies based on optically selected host samples indicate, and that the previously claimed deficiency of high-mass hosts was at least partially a selection effect.

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“…New evidence has shown that GRBs with heavily dust-extinguished afterglows exist in systematically more massive galaxies , thus originally biasing our opinion on host galaxies. Furthermore, it has been seen before that not all GRB host galaxies fit the picture of low-mass, low-metallicity (see e.g., Levesque et al 2010;Hashimoto et al 2010;Savaglio et al 2012) and that some can occur in extremely dust extinguished galaxies Berger et al 2007;Hashimoto et al 2010;Hunt et al 2011, Rossi et al 11), which are also usually associated with large metallicities.…”

Section: Introductionmentioning

confidence: 99%

The longγ-ray burst rate and the correlation with host galaxy properties

Elliott

Greiner

Khochfar

et al. 2012

A&A

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Context. To answer questions on the start and duration of the epoch of reionisation, periods of galaxy mergers and properties of other cosmological encounters, the cosmic star formation history,ρ * or CSFH, is of fundamental importance. Using the association of long-duration gamma-ray bursts (LGRBs) with the death of massive stars and their ultra-luminous nature (>10 52 erg s −1 ), the CSFH can be probed to higher redshifts than current conventional methods. Unfortunately, no consensus has been reached on the manner in which the LGRB rate,ρ grb or LGRBR, traces the CSFH, leaving many of the questions mentioned mostly unexplored by this method. Aims. Observations by the gamma-ray burst near-infrared detector (GROND) over the past 4 years have, for the first time, acquired highly complete LGRB samples. Driven by these completeness levels and new evidence of LGRBs also occurring in more massive and metal rich galaxies than previously thought, the possible biases of theρ grb -ρ * connection are investigated over a large range of galaxy properties. Methods. The CSFH is modelled using empirical fits to the galaxy mass function and galaxy star formation rates. Biasing the CSFH by means of metallicity cuts, mass range boundaries, and other unknown redshift dependencies of the formρ grb ∝ρ * (1 + z) δ , aρ grb is generated and compared to the highly complete GROND LGRB sample. Results. It is found that there is no strong preference for a metallicity cut or fixed galaxy mass boundaries and that there are no unknown redshift effects (δ = 0), in contrast to previous work which suggest values of Z/Z ∼ 0.1−0.3. From the best-fit models obtained, we predict that ∼1.2% of the LGRB burst sample exists above z = 6. Conclusions. The linear relationship betweenρ grb andρ * suggested by our results implies that redshift biases present in previous LGRB samples significantly affect the inferred dependencies of LGRBs on their host galaxy properties. Such biases can lead to, for example, an interpretation of metallicity limitations and evolving LGRB luminosity functions.

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“DARK” GRB 080325 IN A DUSTY MASSIVE GALAXY ATz∼ 2

Cited by 28 publications

References 53 publications

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

The SEDs and host galaxies of the dustiest GRB afterglows

The longγ-ray burst rate and the correlation with host galaxy properties

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