MS 1603.6+2600: an accretion disc corona source?     

P. G. Jonker  M. van der Klis  C. Kouveliotou  M. Méndez  W. H. G. Lewin  T. Belloni 《Monthly notices of the Royal Astronomical Society》2003,346(2):684-688

We have observed the eclipsing low-mass X-ray binary MS 1603.6+2600 with Chandra for 7 ks. The X-ray spectrum is well fit with a single absorbed power law with an index of ∼2. We find a clear sinusoidal modulation in the X-ray light curve with a period of  1.7 ± 0.2 h  , consistent with the period of 1.85 h found before. However, no (partial) eclipses were found. We argue that if the X-ray flare observed in earlier X-ray observations was a type I X-ray burst, then the source can only be an accretion disc corona source at a distance of ∼11–24 kpc (implying a height above the Galactic disc of ∼8–17 kpc). It has also been proposed in the literature that MS 1603.76+2600 is a dipper at ∼75 kpc. We argue that, in this dipper scenario, the observed optical properties of MS 1603.6+2600 are difficult to reconcile with the optical properties one would expect on the basis of comparisons with other high-inclination, low-mass X-ray binaries, unless the X-ray flare was not a type I X-ray burst. In that case, the source can be a nearby soft X-ray transient accreting at a quiescent rate, as was proposed by Hakala et al., or a high-inclination source at ∼15–20 kpc.  相似文献   

ASCA Observation of the Quiescent X-Ray Counterpart to SGR 1627-41     

Hurley K  Strohmayer T  Li P  Kouveliotou C  Woods P  van Paradijs J  Murakami T  Hartmann D  Smith I  Ando M  Yoshida A  Sugizaki M 《The Astrophysical journal》2000,528(1):L21-L23

We present a 2-10 keV ASCA observation of the field around the soft gamma repeater SGR 1627-41. A quiescent X-ray source, whose position is consistent both with that of a recently discovered BeppoSAX X-ray source and with the Interplanetary Network localization for this soft gamma repeater, was detected in this observation. In 2-10 keV X-rays, the spectrum of the X-ray source may be fit equally well by a power-law, blackbody, or bremsstrahlung function, with unabsorbed flux approximately 5x10-12 ergs cm-2 s-1. We do not confirm a continuation of a fading trend in the flux, and we find no evidence for periodicity, both of which were noted in the earlier BeppoSAX observations.  相似文献   

The submillimetre properties of gamma-ray burst host galaxies     

N. R. Tanvir  V. E. Barnard  A. W. Blain  A. S. Fruchter  C. Kouveliotou  P. Natarajan  E. Ramirez-Ruiz  E. Rol  I. A. Smith  R. P. J. Tilanus  R. A. M. J. Wijers 《Monthly notices of the Royal Astronomical Society》2004,352(3):1073-1080

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BACODINE,the real-time BATSE gamma-ray burst coordinates distribution network     

S. D. Barthelmy  P. Butterworth  T. L. Cline  N. Gehrels  G. J. Fishman  C. Kouveliotou  C. A. Meegan 《Astrophysics and Space Science》1995,231(1-2):235-238

The celestial coordinates of gamma-ray burst sources observed with BATSE on GRO are automatically determined and distributed in real time to members of the global scientific community. These data are now being used by more than 20 operations to enable searches for associated transients in a variety of other wavelength or energy regimes to identify the burst source objects. The minimum total delay time from the onset of a burst to the receipt of its coordinates by distant experimenters can be under 4 sec, less than the duration of a typical GRB, and the maximum total delay is 7 sec, or longer, depending on the distribution method. Some improvements to the BACODINE system and a summary of the follow-up observations made by some of the sites are given.  相似文献   

Reproductive traits of the freshwater shrimp Caridina fossarum Heller, 1862 (Decapoda, Caridea, Atyidae) in the Ghomp-Atashkedeh spring (Iran)     

Parviz Zare  Mojtaba Naderi  Hamidreza Eshghi  Chryssa Anastasiadou 《Limnologica》2011,41(3):244-248

In the present study, some biological traits of Caridina fossarum reproduction are studied in the Ghomp-Atashkedeh spring (Fasa, Shiraz, Iran), for the first time. This Iranian endemic freshwater species was studied from April 2007 to March 2008. Minimum sexable size (MSS) and absolute or relative size at the onset of maturity (SOM and RSOM) in terms of carapace length (CL) was found to be 2.4 mm, 4.3 mm and 55%, respectively. Sex ratio showed variations on a monthly basis. Sex reversal is a possible scenario for C. fossarum because the size-specific sex ratio revealed a reverse pattern. Based on the proportions of ovigerous females, the main breeding season was determined to be from April to August, demonstrating a peak during early spring. There is a period of extended recruitment at water temperatures above 20 °C. The size at which 50% of females are mature was estimated at CL = 5.03 mm from the proportion of ovigerous females during the breeding season. The pleopodal egg number varied from 3 to 75 eggs per female with a mean value 34.39 ± 14.27. The results showed that although there is a significant relationship between carapace length CL and pleopodal egg number, it is not the most important factor affecting potential fecundity in C. fossarum due to the low values of slope (= 1.51) and determination coefficient (= 0.052).  相似文献   

Spitzer space telescope observations of SGR and AXP environments     

Stefanie Wachter  Chryssa Kouveliotou  Sandeep Patel  Don Figer  Peter Woods 《Astrophysics and Space Science》2007,308(1-4):67-71

Both Anomalous X-ray Pulsars (AXPs) and Soft Gamma Repeaters (SGRs) are thought to be manifestations of magnetars. However, the specific physical characteristics that differentiate the two classes of objects remain unclear. There is some evidence that the progenitors of these sources and/or the environment in which they form might influence the type of phenomena the resulting magnetar displays. Several of the AXPs appear to be associated with supernova remnants, while embedded clusters of massive stars have been found in the immediate vicinity of some SGRs. Since both AXPs and SGRs are distributed close to the Galactic plane, high extinction makes studies in the optical difficult. We present early results from our Spitzer program aimed at probing the environmental factors that might contribute to the difference in the observed characteristics between AXPs and SGRs.  相似文献   

Spectral evolution of the peculiar Ic Supernova 1998bw     

R. A. Stathakis  B. J. Boyle  D. H. Jones  M. S. Bessell  T. J. Galama  Lisa M. Germany  M. Hartley  D. M. James  C. Kouveliotou  I. J. Lewis  Q. A. Parker  K. S. Russell  E. M. Sadler  C. G. Tinney  J. van Paradijs  P. M. Vreeswijk 《Monthly notices of the Royal Astronomical Society》2000,314(4):807-814

Supernova 1998bw holds the record for the most energetic Type Ic explosion, one of the brightest radio supernovae and probably the first supernova associated with a γ -ray burst. In this paper we present spectral observations of SN 1998bw observed in a cooperative monitoring campaign using the Anglo-Australian Telescope, the UK Schmidt Telescope and the Siding Springs Observatories 2.3-m telescope. We investigate the evolution of the spectrum between 7 and 94 d after V -band maximum in comparison with well-studied examples of Type Ic SNe in order to quantify the unusual properties of this supernova event. Though the early spectra differ greatly from observations of classical Ic supernovae (SNe), we find that the evolution from the photospheric to nebular phases is slow but otherwise typical. The spectra differ predominantly in the extensive line blending and blanketing which has been attributed to the high velocity of the ejecta. We find that by day 19, the absorption line minima blueshifts are 10–50 per cent higher than other SNe and on day 94 emission lines are 45 per cent broader, as expected if the progenitor had a massive envelope. However, it is difficult to explain the extent of line blanketing entirely by line broadening, and we argue that an additional contribution from other species is present, indicating unusual relative abundances or physical conditions in the envelope.  相似文献   

VLA observations of GRB error boxes     

D. M. Palmer  T. L. Cline  J. G. Laros  K. Hurley  G. J. Fishman  C. Kouveliotou 《Astrophysics and Space Science》1995,231(1-2):315-318

Very Large Array (VLA) radio observations of precisely-located GRB error boxes have been performed to search for fading and quiescent emission associated with -ray bursts. These observations were made as quickly as 23 hours and as late as 13 years after the time of the burst. Our measurements presented here have found GRB error boxes to be empty of sources to the 80 µJy level ( = 3.6 cm) at 9 months, to 1 mJy (20 cm) at 9 days, and probably to 5 mJy (20 cm) at 23 hours after the bursts.  相似文献   

Preliminary results of optical searches of IPN3 localizations     

C. B. Luginbuhl  F. J. Vrba  R. Hudec  D. Hartmann  K. Hurley  M. Boër  M. Niel  M. Sommer  C. Kouveliotou  C. Meegan  G. Fishman 《Astrophysics and Space Science》1995,231(1-2):289-292

We present preliminary results from deep optical searches of small (5 arcmin²) GRB error boxes determined using the Third Interplanetary Network (IPN³). Two of these fields also have been found to have historical OT events located within the IPN³ error boxes. We compare the preliminary results of these searches to those reported for the larger IPN¹ error boxes. The small size of the IPN³ error boxes should allow a test of the hypothesis suggested by the IPN¹ study that there are excess QSOs associated with the GRB fields.  相似文献   

Millimetric properties of gamma-ray burst host galaxies     

R. S. Priddey  N. R. Tanvir  A. J. Levan  A. S. Fruchter  C. Kouveliotou  I. A. Smith  R. A. M. J. Wijers 《Monthly notices of the Royal Astronomical Society》2006,369(3):1189-1195

We present millimetre (mm) and submillimetre (submm) photometry of a sample of five host galaxies of gamma-ray bursts (GRBs), obtained using the Max Planck Millimetre Bolometer (MAMBO2) array and Submillimetre Common-User Bolometer Array (SCUBA). These observations were obtained as part of an ongoing project to investigate the status of GRBs as indicators of star formation. Our targets include two of the most unusual GRB host galaxies, selected as likely candidate submm galaxies: the extremely red  ( R − K ≈ 5)  host of GRB 030115, and the extremely faint  ( R > 29.5)  host of GRB 020124. Neither of these galaxies is detected, but the deep upper limits for GRB 030115 impose constraints on its spectral energy distribution, requiring a warmer dust temperature than is commonly adopted for submillimetre galaxies (SMGs).
As a framework for interpreting these data, and for predicting the results of forthcoming submm surveys of Swift -derived host samples, we model the expected flux and redshift distributions based on luminosity functions of both submm galaxies and GRBs, assuming a direct proportionality between the GRB rate density and the global star formation rate density. We derive the effects of possible sources of uncertainty in these assumptions, including (1) introducing an anticorrelation between GRB rate and the global average metallicity, and (2) varying the dust temperature.  相似文献