X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912

G. Stratta; S. Basa; N. Butler; J. L. Atteia; B. Gendre; A. Pelangeon; F. Malacrino; Y. Mellier; D. A. Kann; S. Klose; A. Zeh; N. Masetti; E. Palazzi; J. Gorosabel; A. J. Castro-Tirado; A. de Ugarte Postigo; M. Jelinek; J. Cepa; H. Castaneda; D. Martinez-Delgado; M. Boer; J. Braga; G. Crew; T. Q. Donaghy; J. -P. Dezalay; J. Doty; E. E. Fenimore; M. Galassi; C. Graziani; J. G. Jernigan; N. Kawai; D. Q. Lamb; A. Levine; R. K. Manchanda; F. Martel; M. Matsuoka; Y. Nakagawa; J. -F. Olive; G. Pizzichini; G. Prigozhin; G. Ricker; T. Sakamoto; Y. Shirasaki; S. Sugita; M. Suzuki; K. Takagishi; T. Tamagawa; R. Vanderspek; J. Villasenor; S. E. Woosley; M. Yamauchi; A. Yoshida

doi:10.1051/0004-6361:20065831

X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912

G. Stratta, S. Basa, N. Butler, J. L. Atteia, B. Gendre, A. Pelangeon, F. Malacrino, Y. Mellier, D. A. Kann, S. Klose, A. Zeh, N. Masetti, E. Palazzi, J. Gorosabel, A. J. Castro-Tirado, A. de Ugarte Postigo, M. Jelinek, J. Cepa, H. Castaneda, D. Martinez-DelgadoM. Boer, J. Braga, G. Crew, T. Q. Donaghy, J. -P. Dezalay, J. Doty, E. E. Fenimore, M. Galassi, C. Graziani, J. G. Jernigan, N. Kawai, D. Q. Lamb, A. Levine, R. K. Manchanda, F. Martel, M. Matsuoka, Y. Nakagawa, J. -F. Olive, G. Pizzichini, G. Prigozhin, G. Ricker, T. Sakamoto, Y. Shirasaki, S. Sugita, M. Suzuki, K. Takagishi, T. Tamagawa, R. Vanderspek, J. Villasenor, S. E. Woosley, M. Yamauchi, A. Yoshida

Research output: Contribution to journal › Article › peer-review

11 Citations (Web of Science)

Abstract

Context. The origin of X-ray Flashes (XRFs) is still a mystery and several models have been proposed. To disentangle among these models, an important observational tool is the measure of the XRF distance scale, so far available only for a few of them.

Aims. In this work, we present a multi-wavelength study of XRF 040912, aimed at measuring its distance scale and the intrinsic burst properties.

Methods. We performed a detailed spectral and temporal analysis of both the prompt and the afterglow emission and we estimated the distance scale of the likely host galaxy. We then used the currently available sample of XRFs with known distance to discuss the connection between XRFs and classical Gamma-ray Bursts (GRBs).

Results. We found that the prompt emission properties unambiguously identify this burst as an XRF, with an observed peak energy of E(p) = 17 +/- 13 keV and a burst fluence ratio S(2-30 keV)/S(30-400) keV > 1. A non-fading optical source with R similar to 24 mag and with an apparently extended morphology is spatially consistent with the X-ray afterglow, likely the host galaxy. XRF 040912 is a very dark burst since no afterglow optical counterpart is detected down to R > 25 mag (3 sigma limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 angstrom to 10 000 angstrom, shows a single emission line at 9552 angstrom. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Ly alpha cut-off down to 3800 angstrom are consistent with the hypothesis of the [OII] line at redshift z = 1.563 +/- 0.001. The intrinsic spectral properties rank this XRF among the soft GRBs in the E(peak)-E(iso) diagram. Similar results were obtained for most XRFs at known redshift. Only XRF 060218 and XRF 020903 represent a good example of instrinsic XRF (i-XRF) and are possibly associated with a different progenitor population. This scenario may call for a new definition of XRFs.

Original language	English
Pages (from-to)	485-492
Number of pages	8
Journal	Astronomy & Astrophysics
Volume	461
Issue number	2
DOIs	https://doi.org/10.1051/0004-6361:20065831
Publication status	Published - Jan 2007
Externally published	Yes

Access to Document

10.1051/0004-6361:20065831

Cite this

Stratta, G., Basa, S., Butler, N., Atteia, J. L., Gendre, B., Pelangeon, A., Malacrino, F., Mellier, Y., Kann, D. A., Klose, S., Zeh, A., Masetti, N., Palazzi, E., Gorosabel, J., Castro-Tirado, A. J., Postigo, A. D. U., Jelinek, M., Cepa, J., Castaneda, H., ... Yoshida, A. (2007). X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912. Astronomy & Astrophysics, 461(2), 485-492. https://doi.org/10.1051/0004-6361:20065831

@article{bde858ecdfc8476daa34069af60deaa2,

title = "X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912",

abstract = "Context. The origin of X-ray Flashes (XRFs) is still a mystery and several models have been proposed. To disentangle among these models, an important observational tool is the measure of the XRF distance scale, so far available only for a few of them.Aims. In this work, we present a multi-wavelength study of XRF 040912, aimed at measuring its distance scale and the intrinsic burst properties.Methods. We performed a detailed spectral and temporal analysis of both the prompt and the afterglow emission and we estimated the distance scale of the likely host galaxy. We then used the currently available sample of XRFs with known distance to discuss the connection between XRFs and classical Gamma-ray Bursts (GRBs).Results. We found that the prompt emission properties unambiguously identify this burst as an XRF, with an observed peak energy of E(p) = 17 +/- 13 keV and a burst fluence ratio S(2-30 keV)/S(30-400) keV > 1. A non-fading optical source with R similar to 24 mag and with an apparently extended morphology is spatially consistent with the X-ray afterglow, likely the host galaxy. XRF 040912 is a very dark burst since no afterglow optical counterpart is detected down to R > 25 mag (3 sigma limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 angstrom to 10 000 angstrom, shows a single emission line at 9552 angstrom. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Ly alpha cut-off down to 3800 angstrom are consistent with the hypothesis of the [OII] line at redshift z = 1.563 +/- 0.001. The intrinsic spectral properties rank this XRF among the soft GRBs in the E(peak)-E(iso) diagram. Similar results were obtained for most XRFs at known redshift. Only XRF 060218 and XRF 020903 represent a good example of instrinsic XRF (i-XRF) and are possibly associated with a different progenitor population. This scenario may call for a new definition of XRFs.",

keywords = "gamma rays : bursts, HOST GALAXY, STAR-FORMATION, SUPERNOVA, REDSHIFT, DUST, XRF-020903, AFTERGLOW, SPECTRA, STELLAR, 2006AJ",

author = "G. Stratta and S. Basa and N. Butler and Atteia, {J. L.} and B. Gendre and A. Pelangeon and F. Malacrino and Y. Mellier and Kann, {D. A.} and S. Klose and A. Zeh and N. Masetti and E. Palazzi and J. Gorosabel and Castro-Tirado, {A. J.} and Postigo, {A. de Ugarte} and M. Jelinek and J. Cepa and H. Castaneda and D. Martinez-Delgado and M. Boer and J. Braga and G. Crew and Donaghy, {T. Q.} and Dezalay, {J. -P.} and J. Doty and Fenimore, {E. E.} and M. Galassi and C. Graziani and Jernigan, {J. G.} and N. Kawai and Lamb, {D. Q.} and A. Levine and Manchanda, {R. K.} and F. Martel and M. Matsuoka and Y. Nakagawa and Olive, {J. -F.} and G. Pizzichini and G. Prigozhin and G. Ricker and T. Sakamoto and Y. Shirasaki and S. Sugita and M. Suzuki and K. Takagishi and T. Tamagawa and R. Vanderspek and J. Villasenor and Woosley, {S. E.} and M. Yamauchi and A. Yoshida",

year = "2007",

month = jan,

doi = "10.1051/0004-6361:20065831",

language = "English",

volume = "461",

pages = "485--492",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

number = "2",

}

Stratta, G, Basa, S, Butler, N, Atteia, JL, Gendre, B, Pelangeon, A, Malacrino, F, Mellier, Y, Kann, DA, Klose, S, Zeh, A, Masetti, N, Palazzi, E, Gorosabel, J, Castro-Tirado, AJ, Postigo, ADU, Jelinek, M, Cepa, J, Castaneda, H, Martinez-Delgado, D, Boer, M, Braga, J, Crew, G, Donaghy, TQ, Dezalay, J-P, Doty, J, Fenimore, EE, Galassi, M, Graziani, C, Jernigan, JG, Kawai, N, Lamb, DQ, Levine, A, Manchanda, RK, Martel, F, Matsuoka, M, Nakagawa, Y, Olive, J-F, Pizzichini, G, Prigozhin, G, Ricker, G, Sakamoto, T, Shirasaki, Y, Sugita, S, Suzuki, M, Takagishi, K, Tamagawa, T, Vanderspek, R, Villasenor, J, Woosley, SE, Yamauchi, M & Yoshida, A 2007, 'X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912', Astronomy & Astrophysics, vol. 461, no. 2, pp. 485-492. https://doi.org/10.1051/0004-6361:20065831

TY - JOUR

T1 - X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912

AU - Stratta, G.

AU - Basa, S.

AU - Butler, N.

AU - Atteia, J. L.

AU - Gendre, B.

AU - Pelangeon, A.

AU - Malacrino, F.

AU - Mellier, Y.

AU - Kann, D. A.

AU - Klose, S.

AU - Zeh, A.

AU - Masetti, N.

AU - Palazzi, E.

AU - Gorosabel, J.

AU - Castro-Tirado, A. J.

AU - Postigo, A. de Ugarte

AU - Jelinek, M.

AU - Cepa, J.

AU - Castaneda, H.

AU - Martinez-Delgado, D.

AU - Boer, M.

AU - Braga, J.

AU - Crew, G.

AU - Donaghy, T. Q.

AU - Dezalay, J. -P.

AU - Doty, J.

AU - Fenimore, E. E.

AU - Galassi, M.

AU - Graziani, C.

AU - Jernigan, J. G.

AU - Kawai, N.

AU - Lamb, D. Q.

AU - Levine, A.

AU - Manchanda, R. K.

AU - Martel, F.

AU - Matsuoka, M.

AU - Nakagawa, Y.

AU - Olive, J. -F.

AU - Pizzichini, G.

AU - Prigozhin, G.

AU - Ricker, G.

AU - Sakamoto, T.

AU - Shirasaki, Y.

AU - Sugita, S.

AU - Suzuki, M.

AU - Takagishi, K.

AU - Tamagawa, T.

AU - Vanderspek, R.

AU - Villasenor, J.

AU - Woosley, S. E.

AU - Yamauchi, M.

AU - Yoshida, A.

PY - 2007/1

Y1 - 2007/1

N2 - Context. The origin of X-ray Flashes (XRFs) is still a mystery and several models have been proposed. To disentangle among these models, an important observational tool is the measure of the XRF distance scale, so far available only for a few of them.Aims. In this work, we present a multi-wavelength study of XRF 040912, aimed at measuring its distance scale and the intrinsic burst properties.Methods. We performed a detailed spectral and temporal analysis of both the prompt and the afterglow emission and we estimated the distance scale of the likely host galaxy. We then used the currently available sample of XRFs with known distance to discuss the connection between XRFs and classical Gamma-ray Bursts (GRBs).Results. We found that the prompt emission properties unambiguously identify this burst as an XRF, with an observed peak energy of E(p) = 17 +/- 13 keV and a burst fluence ratio S(2-30 keV)/S(30-400) keV > 1. A non-fading optical source with R similar to 24 mag and with an apparently extended morphology is spatially consistent with the X-ray afterglow, likely the host galaxy. XRF 040912 is a very dark burst since no afterglow optical counterpart is detected down to R > 25 mag (3 sigma limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 angstrom to 10 000 angstrom, shows a single emission line at 9552 angstrom. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Ly alpha cut-off down to 3800 angstrom are consistent with the hypothesis of the [OII] line at redshift z = 1.563 +/- 0.001. The intrinsic spectral properties rank this XRF among the soft GRBs in the E(peak)-E(iso) diagram. Similar results were obtained for most XRFs at known redshift. Only XRF 060218 and XRF 020903 represent a good example of instrinsic XRF (i-XRF) and are possibly associated with a different progenitor population. This scenario may call for a new definition of XRFs.

AB - Context. The origin of X-ray Flashes (XRFs) is still a mystery and several models have been proposed. To disentangle among these models, an important observational tool is the measure of the XRF distance scale, so far available only for a few of them.Aims. In this work, we present a multi-wavelength study of XRF 040912, aimed at measuring its distance scale and the intrinsic burst properties.Methods. We performed a detailed spectral and temporal analysis of both the prompt and the afterglow emission and we estimated the distance scale of the likely host galaxy. We then used the currently available sample of XRFs with known distance to discuss the connection between XRFs and classical Gamma-ray Bursts (GRBs).Results. We found that the prompt emission properties unambiguously identify this burst as an XRF, with an observed peak energy of E(p) = 17 +/- 13 keV and a burst fluence ratio S(2-30 keV)/S(30-400) keV > 1. A non-fading optical source with R similar to 24 mag and with an apparently extended morphology is spatially consistent with the X-ray afterglow, likely the host galaxy. XRF 040912 is a very dark burst since no afterglow optical counterpart is detected down to R > 25 mag (3 sigma limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 angstrom to 10 000 angstrom, shows a single emission line at 9552 angstrom. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Ly alpha cut-off down to 3800 angstrom are consistent with the hypothesis of the [OII] line at redshift z = 1.563 +/- 0.001. The intrinsic spectral properties rank this XRF among the soft GRBs in the E(peak)-E(iso) diagram. Similar results were obtained for most XRFs at known redshift. Only XRF 060218 and XRF 020903 represent a good example of instrinsic XRF (i-XRF) and are possibly associated with a different progenitor population. This scenario may call for a new definition of XRFs.

KW - gamma rays : bursts

KW - HOST GALAXY

KW - STAR-FORMATION

KW - SUPERNOVA

KW - REDSHIFT

KW - DUST

KW - XRF-020903

KW - AFTERGLOW

KW - SPECTRA

KW - STELLAR

KW - 2006AJ

U2 - 10.1051/0004-6361:20065831

DO - 10.1051/0004-6361:20065831

M3 - Article

SN - 0004-6361

VL - 461

SP - 485

EP - 492

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

IS - 2

ER -

X-ray flashes or soft gamma-ray bursts? The case of the likely distant XRF 040912

Abstract

Access to Document

Fingerprint

Cite this