| 11. |
- D'Elia, V., et al.
(author)
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VLT/X-shooter spectroscopy of the GRB 090926A afterglow
- 2010
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In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 523, s. 36-
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Journal article (peer-reviewed)abstract
- Aims: The aim of this paper is to study the environment and intervening absorbers of the gamma-ray burst GRB 090926A through analyzing optical spectra of its afterglow. Methods: We analyzed medium-resolution spectroscopic observations (R = 10 000, corresponding to 30 km s-1, S/N = 15-30 and wavelength range 3000-25 000) of the optical afterglow of GRB 090926A, taken with X-shooter at the VLT ~22 h after the GRB trigger. Results: The spectrum shows that the ISM in the GRB host galaxy at z = 2.1071 is rich in absorption features, with two components contributing to the line profiles. In addition to the ground state lines, we detect C ii, O i, Si ii, Fe ii, and Ni ii-excited absorption features, which we used to derive information on the distance between the host absorbing gas and the site of the GRB explosion. The distance of component I is found to be 2.40 ± 0.15 kpc, while component II is located far away from the GRB, possibly at ~5 kpc. These values are compatible with those found for other GRBs. The hydrogen column density associated to GRB 090926A is log NH/cm -2 = 21.60 ± 0.07, and the metallicity of the host galaxy is in the range [X/H] = -2.5 to -1.9 with respect to the solar values, i.e., among the lowest values ever observed for a GRB host galaxy. A comparison with galactic chemical evolution models has suggested that the host of GRB090926A is likely to be a dwarf-irregular galaxy. No emission lines were detected, but a Hα flux in emission of 9 × 10-18 erg s-1 cm-2 (i.e., a star-formation rate of 2 M_ȯ yr-1), which is typical of many GRB hosts, would have been detected in our spectra, and thus emission lines are well within the reach of X-shooter. We put an upper limit to the H molecular fraction of the host galaxy ISM, which is f < 7 × 10-7. The continuum has been fitted assuming a power-law spectrum, with a spectral index of β = 0.89-0.02+0.02. The best fit does essentially not require any intrinsic extinction because EB-V < 0.01 mag adopting a SMC extinction curve. Finally, the line of sight of GRB 090926A presents four weak intervening absorption systems in the redshift range 1.24 < z < 1.95. Based on observations collected at the European Southern Observatory, ESO, the VLT/Kueyen telescope, Paranal, Chile, during the science verification phase, proposal code: 060-9427(A).
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| 12. |
- Vajta, Zs., et al.
(author)
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Excited states in the neutron-rich nucleus F-25
- 2014
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In: Physical Review C. Nuclear Physics. - 0556-2813 .- 1089-490X. ; 89:5, s. 054323-
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Journal article (peer-reviewed)abstract
- The structure of the nucleus F-25(9) was investigated through in-beam. gamma-ray spectroscopy of the fragmentation of Ne-26 and Na-27,Na-28 ion beams. Based on the particle-gamma and particle-gamma gamma coincidence data, a level scheme was constructed and compared with shell model and coupled-cluster calculations. Some of the observed states were interpreted as quasi-single-particle states built on top of the closed-shell nucleus O-24, while the others were described as states arising from coupling of a single proton to the 2(broken vertical bar) core excitation of O-24.
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| 13. |
- Cano, Z., et al.
(author)
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A trio of gamma-ray burst supernovae : GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu
- 2014
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In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 568
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Journal article (peer-reviewed)abstract
- We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. For GRB 130215A/SN 2013ez, we also present optical spectroscopy at t-t(0) = 16.1 d, which covers rest-frame 3000-6250 angstrom. Based on Fell lambda 5169 and Sill lambda 6355, our spectrum indicates an unusually low expansion velocity of similar to 4000-6350 km s(-1), the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A/SN 2013fu, we used our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we took advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Meszros (2001, ApJ, 552, L35), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P = 12 ms and a magnetic field of B = 1.1 x 10(15) G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs.
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| 14. |
- Gimsing, Peter, et al.
(author)
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Effect of pamidronate 30 mg versus 90 mg on physical function in patients with newly diagnosed multiple myeloma (Nordic Myeloma Study Group): a double-blind, randomised controlled trial
- 2010
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In: LANCET ONCOLOGY. - : Elsevier Science B.V., Amsterdam.. - 1470-2045 .- 1474-5488. ; 11:10, s. 973-982
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Journal article (peer-reviewed)abstract
- Background Compared with placebo, prophylactic treatment with bisphosphonates reduces risk of skeletal events in patients with multiple myeloma. However, because of toxicity associated with long-term bisphosphonate treatment, establishing the lowest effective dose is important. This study compared the effect of two doses of pamidronate on health-related quality of life and skeletal morbidity in patients with newly diagnosed multiple myeloma. Methods This double-blind, randomised, phase 3 trial was undertaken at 37 clinics in Denmark, Norway, and Sweden. Patients with multiple myeloma who were starting antimyeloma treatment were randomly assigned in a 1:1 ratio to receive one of two doses of pamidronate (30 mg or 90 mg) given by intravenous infusion once a month for at least 3 years. Randomisation was done by use of a central, computerised minimisation system. Primary outcome was physical function after 12 months estimated by the European Organisation for Research and Treatment of Cancer (EORTC) QLQ-C30 questionnaire (scale 0-100). All patients who returned questionnaires at 12 months and were still on study treatment were included in the analysis of the primary endpoint. This study is registered with ClinicalTrials. gov, number NCT00376883. Findings From January, 2001, until August, 2005, 504 patients were randomly assigned to pamidronate 30 mg or 90 mg (252 in each group). 157 patients in the 90 mg group and 156 in the 30 mg group were included in the primary analysis. Mean physical function at 12 months was 66 points (95% CI 62.9-70.0) in the 90 mg group and 68 points (64.6-71.4) in the 30 mg group (95% CI of difference -6.6 to 3.3; p=0.52). Median time to first skeletal-related event in patients who had such an event was 9.2 months (8.1-10.7) in the 90 mg group and 10-2 months (7.3-14.0) in the 30 mg group (p=0.63). In a retrospective analysis, eight patients in the pamidronate 90 mg group developed osteonecrosis of the jaw compared with two patients in the 30 mg group. Interpretation Monthly infusion of pamidronate 30 mg should be the recommended dose for prevention of bone disease in patients with multiple myeloma.
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| 15. |
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| 16. |
- Margutti, R., et al.
(author)
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A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE
- 2014
-
In: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 780:1
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Journal article (peer-reviewed)abstract
- The double explosion of SN 2009ip in 2012 raises questions about our understanding of the late stages of massive star evolution. Here we present a comprehensive study of SN 2009ip during its remarkable rebrightenings. High-cadence photometric and spectroscopic observations from the GeV to the radio band obtained from a variety of ground-based and space facilities (including the Very Large Array, Swift, Fermi, Hubble Space Telescope, and XMM) constrain SN 2009ip to be a low energy (E similar to 1050 erg for an ejecta mass similar to 0.5 M-circle dot) and asymmetric explosion in a complex medium shaped by multiple eruptions of the restless progenitor star. Most of the energy is radiated as a result of the shock breaking out through a dense shell of material located at similar to 5 x 10(14) cm with M similar to 0.1 M-circle dot, ejected by the precursor outburst similar to 40 days before the major explosion. We interpret the NIR excess of emission as signature of material located further out, the origin of which has to be connected with documented mass-loss episodes in the previous years. Our modeling predicts bright neutrino emission associated with the shock break-out if the cosmic-ray energy is comparable to the radiated energy. We connect this phenomenology with the explosive ejection of the outer layers of the massive progenitor star, which later interacted with material deposited in the surroundings by previous eruptions. Future observations will reveal if the massive luminous progenitor star survived. Irrespective of whether the explosion was terminal, SN 2009ip brought to light the existence of new channels for sustained episodic mass loss, the physical origin of which has yet to be identified.
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| 17. |
- Michalowski, M. J., et al.
(author)
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THE OPTICALLY UNBIASED GRB HOST (TOUGH) SURVEY. VI. RADIO OBSERVATIONS AT z less than or similar to 1 AND CONSISTENCY WITH TYPICAL STAR-FORMING GALAXIES
- 2012
-
In: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 755:2, s. 85-
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Journal article (peer-reviewed)abstract
- The objective of this paper is to determine the level of obscured star formation activity and dust attenuation in a sample of gamma-ray burst (GRB) hosts, and to test the hypothesis that GRB hosts have properties consistent with those of the general star-forming galaxy populations. We present a radio continuum survey of all z < 1 GRB hosts in The Optically Unbiased GRB Host (TOUGH) sample supplemented with radio data for all (mostly pre-Swift) GRB-SN hosts discovered before 2006 October. We present new radio data for 22 objects and have obtained a detection for three of them (GRB 980425, 021211, 031203; none in the TOUGH sample), increasing the number of radio-detected GRB hosts from two to five. The star formation rate (SFR) for the GRB 021211 host of similar to 825 M-circle dot yr(-1), the highest ever reported for a GRB host, places it in the category of ultraluminous infrared galaxies. We found that at least similar to 63% of GRB hosts have SFR < 100 M-circle dot yr(-1) and at most similar to 8% can have SFR > 500 M-circle dot yr(-1). For the undetected hosts the mean radio flux (<35 mu Jy 3 sigma) corresponds to an average SFR < 15 M-circle dot yr(-1). Moreover, greater than or similar to 88% of the z less than or similar to 1 GRB hosts have ultraviolet dust attenuation A(UV) < 6.7 mag (visual attenuation A(V) < 3 mag). Hence, we did not find evidence for large dust obscuration in a majority of GRB hosts. Finally, we found that the distributions of SFRs and A(UV) of GRB hosts are consistent with those of Lyman break galaxies, H alpha emitters at similar redshifts, and of galaxies from cosmological simulations. The similarity of the GRB population with other star-forming galaxies is consistent with the hypothesis that GRBs, a least at z less than or similar to 1, trace a large fraction of all star formation, and are therefore less biased indicators than once thought.
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| 18. |
- Mustjoki, S, et al.
(author)
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Impact of malignant stem cell burden on therapy outcome in newly diagnosed chronic myeloid leukemia patients
- 2013
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In: Leukemia. - : Springer Science and Business Media LLC. - 0887-6924 .- 1476-5551. ; 27:7, s. 1520-1526
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Journal article (peer-reviewed)abstract
- Chronic myeloid leukemia (CML) stem cells appear resistant to tyrosine kinase inhibitors (TKIs) in vitro, but their impact and drug sensitivity in vivo has not been systematically assessed. We prospectively analyzed the proportion of Philadelphia chromosome-positive leukemic stem cells (LSCs, Ph+CD34+CD38=) and progenitor cells (LPCs, Ph+CD34+CD38+) from 46 newly diagnosed CML patients both at the diagnosis and during imatinib or dasatinib therapy (ClinicalTrials.gov NCT00852566). At diagnosis, the proportion of LSCs varied markedly (1-100%) between individual patients with a significantly lower median value as compared with LPCs (79% vs 96%, respectively, P = 0.0001). The LSC burden correlated with leukocyte count, spleen size, hemoglobin and blast percentage. A low initial LSC percentage was associated with less therapy-related hematological toxicity and superior cytogenetic and molecular responses. After initiation of TKI therapy, the LPCs and LSCs rapidly decreased in both therapy groups, but at 3 months time point the median LPC level was significantly lower in dasatinib group compared with imatinib patients (0.05% vs 0.68%, P = 0.032). These data detail for the first time the prognostic significance of the LSC burden at diagnosis and show that in contrast to in vitro data, TKI therapy rapidly eradicates the majority of LSCs in patients.
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| 19. |
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| 20. |
- Sparre, M., et al.
(author)
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SPECTROSCOPIC EVIDENCE FOR SN 2010ma ASSOCIATED WITH GRB 101219B
- 2011
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In: The Astrophysical Journal Letters. - 2041-8205. ; 735:1, s. L24-
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Journal article (peer-reviewed)abstract
- We report on the spectroscopic detection of supernova SN 2010ma associated with the long gamma-ray burst GRB 101219B. We observed the optical counterpart of the GRB on three nights with the X-shooter spectrograph at the Very Large Telescope. From weak absorption lines, we measure a redshift of z = 0.55. The first-epoch UV-near-infrared afterglow spectrum, taken 11.6 hr after the burst, is well fit by a power law consistent with the slope of the X-ray spectrum. The second-and third-epoch spectra (obtained 16.4 and 36.7 days after the burst), however, display clear bumps closely resembling those of the broad-lined type-Ic SN 1998bw if placed at z = 0.55. Apart from demonstrating that spectroscopic SN signatures can be observed for GRBs at these large distances, our discovery makes a step forward in establishing a general connection between GRBs and SNe. In fact, unlike most previous unambiguous GRB-associated SNe, GRB 101219B has a large gamma-ray energy (E(iso) = 4.2x10(51) erg), a bright afterglow, and obeys the Amati relation, thus being fully consistent with the cosmological population of GRBs.
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