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Scientific Highlights of the HETE-2 Mission. D. Q. Lamb (U. Chicago). Los Alamos National Laboratory Los Alamos, NM USA. Center for Space Research Massachusetts Institute of Technology Cambridge, MA USA. Edward E. Fenimore Mark Galassi. George R. Ricker (PI) Geoffrey B. Crew - PowerPoint PPT Presentation
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Scientific Highlights of the HETE-2 Mission
D. Q. Lamb (U. Chicago)
HETE-2 International Science Team
Cosmic Radiation Laboratory Institute of Physical and Chemical Research
(RIKEN)JAPAN
Masaru Matsuoka Nobuyuki Kawai Atsumasa Yoshida
Centre D’Etude Spatiale des Rayonnements (CESR)
FRANCE
Jean-Luc Atteia Michel Boer Gilbert Vedrenne
Brazil + India + Italy (Burst Alert Station Scientists)
Joao BragaRavi ManchandaGraziella Pizzichini
Los Alamos National Laboratory
Los Alamos, NM USA
Edward E. FenimoreMark Galassi
Space Science LaboratoryUniversity of California at Berkeley, CA
USA
Kevin Hurley J. Garrett Jernigan
Astronomy and Astrophysics Department University of Chicago, IL USA
Donald Q. Lamb Jr.Carlo GrazianiTim Donaghy
Board of Astronomy and Astrophysics University of California at Santa Cruz, CA
USA
Stanford E. Woosley
Thomas L.Cline (NASA Project Scientist)
Goddard Space Flight Center Greenbelt, MDUSA
Center for Space Research Massachusetts Institute of TechnologyCambridge, MA USA
George R. Ricker (PI)Geoffrey B. Crew John P. Doty
Alan M. Levine Roland K. VanderspekJoel Villasenor
(Mission Scientist)
Outline of This Talk
In this talk, I will discuss the implications of HETE-2 and follow-up observations for:
Short, hard GRBs GRB afterglows as a probe of the circumburst
environment “Optically dark GRBs” X-ray-rich GRBs and X-Ray Flashes (XRFs)
HETE-2 Observations of GRB 020531
BeppoSAX did not detect any short GRBs in its 6-year mission lifetime, despite extensive efforts
GRB 020531 is first observation of short GRB that has allowed rapid follow-up observations (previous best was > 2 weeks).
GRB020531: Light Curves in 4 Energy Bands
6-13 keV 30-85 keV
85-300 keV(t50= 360ms)
13-30 keV
Lamb et al. (2002)
Spectrum of GRB020531Lamb et al. (2002)
Spectrum is relatively soft for a short, hard GRB (alpha = 1.26 +/- 0.05, E_peak = 170 +/- 20 keV)
GRB020531: Strong Spectral Evolution
Power law x exponential adequately fits spectrum of both of the time intervals t_1 = 0 - 0.8 s and t_2 = 0.8 – 1.3 s
Solid curves are 1-, 2-, and 3-sigma contours for t_1 Dashed and dash-dotted curves are same for t_2
GRB020531: Strong Spectral Evolution
Probability that there isProbability that there is nono changechange in spectral in spectral slope = 1.4 x 10^-3slope = 1.4 x 10^-3
GRB020531: Duration Increases as Energy Decreases
Lamb et al. (2002)
GRB020531: Implications
HETE-2 observations show that this short, hard burst is similar to long bursts in several ways: Exhibits strong spectral evolution from hard to soft Duration increases toward lower energies as E^-alpha with
alpha ~ 0.4 Has a soft tail, lasting ~ 6 seconds
Similarity of these properties to those of long bursts suggests similar or same emission mechanism, and possibly same central engine
Rapid Follow-Up Observations of GRB 020531
GRB020531: Implications
Rapid HETE-2 and IPN localizations made possible rapid optical (t = 2 - 3 hrs) follow-up observations (previous best was t > 2 weeks) Chandra observations at t = 5 days => this short GRB
not associated with a fading X-ray source (C00 or C48) not associated with a slow-fading optical source (C05) not associated with high-redshift galaxy (C48)
L_x (short)/L_x (long) < 0.01 - 0.03 @ t = 5 days Suggests there may be great premium on real time or
near-real time X-ray follow-up observations of short GRBs
HETE-2 Observations of GRB 020813
Long, bright GRB. HETE-2 localized GRB in near-real time.
HETE-2 Observations of GRB 020819
HETE-2 localized GRB in near-real time. Example of “optically dark” GRB.
GRB021004: Structure of Circumburst Medium
GRB021004: T + 43 sec
GRB021004: T + 73 min
GRB021004: T + 154 min
GRB021004: T + 180 min(Optical Transient Detected at T + 9 min)
Discovery of GRB 021004 Optical Afterglow
Observations using 48” Schmidt telescope at Palomar Observatory began 9 minutes after start of GRB.
Spectroscopic observations < 3 hours later gave first redshift info (z > 1.6) on burst.
Optical afterglow very bright (R = 15.4) at discovery.
GRB 021004 Optical Afterglow Light Curve
Follow-up observations made by > 100 telescopes worldwide.
Early observations may show effect of “forward shock” encountering variations (“clumping”) of medium immediately surrounding GRB
GRB afterglows provide info on last years - days of life of (massive) pre-supernova star
Many unexplained bumps in optical afterglow light curve.
Radio afterglow has strange spectrum.
GRB 021004 Optical Afterglow Spectrum
Redshift of GRB (and its host galaxy) are z = 2.32 Spectrum reveals cloud structure in host galaxy Many absorption lines produced by metals in galaxies and gas clouds
along line-of-sight between GRB and us Provides info on metallicity history of universe out to redshift of GRB
Change in GRB 021004 Afterglow Spectrum
Spectrum of optical afterglow reddened significantly in < 1 day (expected in most popular model, due to electron cooling, but
this is1st time such a change has been directly observed).
“Optically Dark” GRBs
HETE-2 is solving the mystery of “optically dark” GRBs Two explanations have been widely discussed:
GRBs lie at very high redshifts (Lamb and Reichart 2000) Optical afterglows are extinguished by dust in the host galaxy
(see, e.g., Reichart and Price 2001) Rapid follow-up observations of HETE-2—localized
burst GRB030115 show that this burst is best case to date of extinction by dust
HETE-2 Observations of GRB030115
Follow-Up Network for GRBs Consortium
Currently involves 9 institutions: University of North Carolina (Dan Reichart, Chris Clemens, Mellisa
Nysewander, Jane Moran, et al.) University of Chicago (Don Lamb, Don York, Russet McMillan, et al.) USNO (Arne Henden, et al.) MMT/SAO (Grant Williams, et al.) University of Wyoming (Ron Canterna, Ray Martin, et al.) Thueringer Landessternwarte Tautenburg (Sylvio Close, et al.) Clemson University (Dieter Hartmann, et al.) Elon University (Anthony Crider, et al.) Tenagra Observatories (Michael Schwartz)
Telescopes include ARC 3.5-m @ APO, SAO 90-inch Bok @KPNO, UW 2.3-m @WIRO,1.5-m Kaj Strand @ USNO, 61-inch UA Kuiper @ Steward, TLS 1.34-m Schmidt @ Tautenburg, 1.3-m and 1.0-m @ USNO, 24-inch CU Super-LOTIS @ KPNO
APO Observations of GRB030115
Shown above is an APO i* image taken 3.5 hours after the burst (right panel) and another taken two weeks later (left panel)
Lamb et al. (2003)
APO and USNO Observations of GRB030115
APO observations on 15 Jan 2002 UT began about 4 hours after the burst, measured i* = 22.1 +/- 0.04 (left panel) and r* = 23.40 +/- 0.11 (right panel)
USNO observations also began about 3.5 hours after the burst; measured J = 19.78 +/-0.20, H = 18.28 +/- 0.13 (Henden et al. 2003)
(Lamb et al. 2003)
GRB030115: Evidence for Extinction by Dust
(Lamb et al. 2003)
Chandra follow-up observations crucial: needed to fix slope of afterglow spectrum
GRB030115: Host Galaxy
HETE-2 Observations of GRB021211
Crew et al. (2003)
APO Observations of GRB021211
GRB021211: Host Galaxy
GRB021211: Near Real-Time Afterglow Observations
Li et al. (2003)
GRB021211: Afterglow Light Curve Relative to Those of Other GRBs
Fox et al. (2003)
GRB021211: Implications for “Optically Dark” GRBs
Nature of “optically dark” bursts is largely unknown Two explanations have been widely discussed:
GRBs lie a very high redshifts (Lamb and Reichart 2000) Optical afterglows are extinguished by dust in the host galaxy
(see, e.g., Reichart and Price 2001) Rapid follow-up observations of HETE-2—localized
burst GRB021211 shows that there is a third explanation in the case of some bursts: their optical afterglow is much, much fainter (> mag) than those observed previously (i.e., they are “optically dim” rather than “optically dark”
Even GRBs whose optical afterglows are dim may have very bright optical afterglows at t< 10 min
“X-Ray Flashes”
Heise et al. (2000) discovered bursts in BeppoSAX WFCs that the BeppoSAX GRBM did not see.
“X-Ray Flashes”
Defining “X-ray flashes” as burst for which log (S_x/S_gamma) > 0 (i.e., > 100 times that for “normal” GRBs), ~25% of bursts localized by HETE-2 are XRFs
Nature of XRFs is largely unknown
““Normal”Normal”F_x/F_g < 0.32F_x/F_g < 0.32[20 GRBs][20 GRBs]
““X-Ray Rich”X-Ray Rich”F_x/F_g>0.32F_x/F_g>0.32[17 GRBs][17 GRBs]
X-Ray-Rich GRBs and X-Ray Flashes
There is increasing evidence that GRBs, X-ray-rich GRBs, and XRFs form a continuum: Heise et al. (2000) showed that durations and time histories
of XRFs are similar to those of GRBs; Kippen et al. (2002) showed that E_peak’s and S’s of XRFs lie near the smallest values of these seen for GRBs
Reichart et al. (2002) successfully applied their variability measure to XRFs, and showed that, if the variability measure is an estimator of the isotropic-equivalent L of the XRF (and therefore the redshift), the L’s and z’s of XRFs are similar to those of GRBs
Barraud et al. (2003) showed that the values of (S_gamma, E_peak) and (S_x,S_gamma) for X-ray-rich GRBs form an extension of those for GRBs, using HETE-2 FREGATE data
HETE-2 Observations of GRB020903
Sakamoto et al. (2003)
GRB020903: SpectrumSakamoto et al. (2003)
E_peak = 3.4 kev!
GRB020903: Discovery of Optical Afterglow
Palomar 48-inch Schmidt images: 2002 Sep 6 (left image), 2002 Sep 28 (middle image; subtracted image (right image)
Soderberg et al. (2002)
GRB020903: S_gamma vs. S_x
Sakamoto et al. (2003)
Barraud et al. (2003)
GRB020903: S_gamma vs. E_peakSakamoto et al. (2003)
Barraud et al. (2003)
Amati et al. (2002) Relation: BeppoSAX GRBs
Amati et al. (2002) Relation: HETE-2 GRBs
Sakamoto et al. (2003)
Amati et al. (2003) Relation: BeppoSAX + HETE-2 GRBs
Sakamoto et al. (2003)
GRB020903: Implications
HETE-2 and optical follow-up observations of GRB020903 show that in the case of this XRF: It lies on the extensions of the above distributions It lies on an extension of the Amati et al. (2002) relation It’s host galaxy is copiously producing stars, similar to those
of GRBs It’s host galaxy has a redshift z = 0.25, simlar to those
of GRBs These results provide strong evidence that GRBs,
X-ray-rich GRBs, and X-Ray Flashes are the same phenomenon
Conclusions
HETE-2 has provided important new information about the nature of short, hard GRBs
HETE-2 is solving the mystery of “optically dark” GRBs: Some are expected to lie at very high redshifts (Lamb and Reichart
2000) HETE-2 and follow-up observations of GRB030115 have provided
a”gold-plated” example of a GRB which is “optically” dark because of extinction by dust
HETE-2 and follow-up observations of GRB021211 have shown that the afterglows of some GRBs can be much fainter than those observed previously (i.e., they are “optically dim,” rather than “optically dark”); yet these afterglows can be very bright at t < 10 minutes after the burst
HETE-2 and follow-up observations of GRB020903 have provided strong new evidence that GRBs, X-ray-rich GRBs, and “X-Ray Flashes” are all the same phenomenon