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

G. Stratta, S. Basa, Nathaniel Butler, J. L. Attela, B. Gendre, A. Pélangeon, 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. Castañeda, D. Martínez-DelgadoM. Boër, 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 journalArticle

7 Citations (Scopus)

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 Ep = 17 ± 13 keV and a burst fluence ratio S 2-30 kev/S/S 30-400 kev > 1. A non-fading optical source with R ∼ 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 (3σ limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 Å to 10 000 Å, shows a single emission line at 9552 A. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Lyα cut-off down to 3800 Å 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 Epeak-EMiso 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 languageEnglish (US)
Pages (from-to)485-492
Number of pages8
JournalAstronomy and Astrophysics
Volume461
Issue number2
DOIs
StatePublished - Jan 2007
Externally publishedYes

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gamma ray bursts
flash
x rays
bursts
afterglows
galaxies
temporal analysis
spectral analysis
spectrum analysis
fluence
cut-off
diagram
diagrams

Keywords

  • Gamma rays: bursts

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Stratta, G., Basa, S., Butler, N., Attela, J. L., Gendre, B., Pélangeon, A., ... Yoshida, A. (2007). X-ray flashes or soft gamma-ray bursts? the case of the likely distant XRF 040912. Astronomy and Astrophysics, 461(2), 485-492. https://doi.org/10.1051/0004-6361:20065831

X-ray flashes or soft gamma-ray bursts? the case of the likely distant XRF 040912. / Stratta, G.; Basa, S.; Butler, Nathaniel; Attela, J. L.; Gendre, B.; Pélangeon, A.; Malacrino, F.; Mellier, Y.; Kann, D. A.; Klose, S.; Zeh, A.; Masetti, N.; Palazzi, E.; Gorosabel, J.; Castro-Tirado, A. J.; De Ugarte Postigo, A.; Jelinek, M.; Cepa, J.; Castañeda, H.; Martínez-Delgado, D.; Boër, M.; Braga, J.; Crew, G.; Donaghy, T. Q.; Dezalay, J. P.; Doty, J.; Fenimore, E. E.; Galassi, M.; Graziani, C.; Jernigan, J. G.; Kawai, N.; Lamb, D. Q.; Levine, A.; Manchanda, R. K.; 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, S. E.; Yamauchi, M.; Yoshida, A.

In: Astronomy and Astrophysics, Vol. 461, No. 2, 01.2007, p. 485-492.

Research output: Contribution to journalArticle

Stratta, G, Basa, S, Butler, N, Attela, JL, Gendre, B, Pélangeon, A, Malacrino, F, Mellier, Y, Kann, DA, Klose, S, Zeh, A, Masetti, N, Palazzi, E, Gorosabel, J, Castro-Tirado, AJ, De Ugarte Postigo, A, Jelinek, M, Cepa, J, Castañeda, H, Martínez-Delgado, D, Boër, M, Braga, J, Crew, G, Donaghy, TQ, Dezalay, JP, 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, JF, 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 and Astrophysics, vol. 461, no. 2, pp. 485-492. https://doi.org/10.1051/0004-6361:20065831
Stratta, G. ; Basa, S. ; Butler, Nathaniel ; Attela, J. L. ; Gendre, B. ; Pélangeon, A. ; Malacrino, F. ; Mellier, Y. ; Kann, D. A. ; Klose, S. ; Zeh, A. ; Masetti, N. ; Palazzi, E. ; Gorosabel, J. ; Castro-Tirado, A. J. ; De Ugarte Postigo, A. ; Jelinek, M. ; Cepa, J. ; Castañeda, H. ; Martínez-Delgado, D. ; Boër, M. ; Braga, J. ; Crew, G. ; Donaghy, T. Q. ; Dezalay, J. P. ; Doty, J. ; Fenimore, E. E. ; Galassi, M. ; Graziani, C. ; Jernigan, J. G. ; Kawai, N. ; Lamb, D. Q. ; Levine, A. ; Manchanda, R. K. ; 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, S. E. ; Yamauchi, M. ; Yoshida, A. / X-ray flashes or soft gamma-ray bursts? the case of the likely distant XRF 040912. In: Astronomy and Astrophysics. 2007 ; Vol. 461, No. 2. pp. 485-492.
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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 Ep = 17 ± 13 keV and a burst fluence ratio S 2-30 kev/S/S 30-400 kev > 1. A non-fading optical source with R ∼ 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 (3σ limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 {\AA} to 10 000 {\AA}, shows a single emission line at 9552 A. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Lyα cut-off down to 3800 {\AA} 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 Epeak-EMiso 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.",
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author = "G. Stratta and S. Basa and Nathaniel Butler and Attela, {J. L.} and B. Gendre and A. P{\'e}langeon 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 {De Ugarte Postigo}, A. and M. Jelinek and J. Cepa and H. Casta{\~n}eda and D. Mart{\'i}nez-Delgado and M. Bo{\"e}r 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",
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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, Nathaniel

AU - Attela, J. L.

AU - Gendre, B.

AU - Pélangeon, 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 - De Ugarte Postigo, A.

AU - Jelinek, M.

AU - Cepa, J.

AU - Castañeda, H.

AU - Martínez-Delgado, D.

AU - Boër, 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 Ep = 17 ± 13 keV and a burst fluence ratio S 2-30 kev/S/S 30-400 kev > 1. A non-fading optical source with R ∼ 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 (3σ limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 Å to 10 000 Å, shows a single emission line at 9552 A. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Lyα cut-off down to 3800 Å 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 Epeak-EMiso 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 Ep = 17 ± 13 keV and a burst fluence ratio S 2-30 kev/S/S 30-400 kev > 1. A non-fading optical source with R ∼ 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 (3σ limiting magnitude) at 13.6 h after the burst. The host galaxy spectrum detected from 3800 Å to 10 000 Å, shows a single emission line at 9552 A. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Lyα cut-off down to 3800 Å 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 Epeak-EMiso 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

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