Moderate Asphericity of the SN 2002ic Circumstellar Envelope

The polarization of SN 2002ic interacting with a dense circumstellar envelope is calculated in the context of the asymmetric version of a previously proposed spherical interaction model. The circumstellar envelope is taken to be oblate. The observed polarization (Wang et al. 2004) can be reproduced for an aspect ratio of 0.65-0.7 assuming inclination angles >60 degrees. This model predicts a weak sensitivity of the line profiles to the orientation, in agreement with the absence of significant variations of the line profiles among SN 2002ic-like supernovae. We propose a test for distinguishing between the binary and single star progenitor scenarios based upon the polarization distribution function for the growing sample of these events.Comment: 13 pages, 4 figs., ApJ, accepte

Optical Signatures of Circumstellar Interaction in Type IIP Supernovae

We propose new diagnostics for circumstellar interaction in Type IIP supernovae by the detection of high velocity (HV) absorption features in Halpha and He I 10830 A lines during the photospheric stage. To demonstrate the method, we compute the ionization and excitation of H and He in supernova ejecta taking into account time-dependent effects and X-ray irradiation. We find that the interaction with a typical red supergiant wind should result in the enhanced excitation of the outer layers of unshocked ejecta and the emergence of corresponding HV absorption, i.e. a depression in the blue absorption wing of Halpha and a pronounced absorption of He I 10830 A at a radial velocity of about -10,000 km/s. We identify HV absorption in Halpha and He I 10830 A lines of SN 1999em and in Halpha of SN 2004dj as being due to this effect. The derived mass loss rate is close to 10^{-6} Msun/yr for both supernovae, assuming a wind velocity 10 km/s. We argue that, in addition to the HV absorption formed in the unshocked ejecta, spectra of SN 2004dj and SN 1999em show a HV notch feature that is formed in the cool dense shell (CDS) modified by the Rayleigh-Taylor instability. The CDS results from both shock breakout and radiative cooling of gas that has passed through the reverse shock wave. The notch becomes dominant in the HV absorption during the late photospheric phase, ~60 d. The wind density deduced from the velocity of the CDS is consistent with the wind density found from the HV absorption produced by unshocked ejecta.Comment: 38 pages, 12 figures, ApJ, in pres

Circumstellar interaction in type Ibn supernovae and SN 2006jc

I analyse peculiar properties of light curve and continua of enigmatic Ibn supernovae, including SN 2006jc, and argue in favour of the early strong circumstellar interaction. This interaction explains the high luminosity and fast flux rise of SN 1999cq, while the cool dense shell formed in shocked ejecta can explain the smooth early continuum of SN 2000er and unusual blue continuum of SN 2006jc. The dust is shown to condense in the cool dense shell at about day 50. Monte Carlo modelling of the He I 7065 \AA line profile affected by the dust occultation supports a picture, in which the dust resides in the fragmented cool dense shell, whereas He I lines originate from circumstellar clouds shocked and fragmented in the forward shock wave.Comment: 10 pages, 6 figures, MNRAS accepte

L'implication des cellules de type cellules souches cancéreuses dans la résistance aux drogues du neuroblastome

Le neuroblastome (NB), tumeur spécifique de l'enfant, se situe au second rang en terme de¦fréquence des tumeurs solides dans la population pédiatrique (1). Il dérive des cellules¦primitives de la crête neurale, une population de cellules embryonnaires dotées d'une¦capacité de différentiation en une panoplie de tissus très variés, dont le système nerveux¦sympathique (2). Cette origine explique la très grande hétérogénéité du NB, tant du point de¦vue biologique que clinique (3). Malgré un traitement intensif et multimodal (chirurgie,¦chimiothérapie à haute dose, greffe de moelle osseuse et immunothérapie), seuls 30 % des¦patients de haut risque (stade IV) survivent sans rechute. La forte résistance du¦neuroblastome de haut grade aux diverses thérapies est une des causes probable du¦pronostic sombre de cette tumeur. Les thérapies actuelles étant insuffisamment efficaces, il¦est primordial de comprendre les mécanismes impliqués dans le processus de résistance¦afin d'élaborer de nouveaux traitements, mieux ciblés, capables de contrer toute résistance¦(4).¦Il a été démontré que certains cancers, tels que les tumeurs du poumon, du sein, de la¦prostate ou du colon, possédaient des cellules souches cancéreuses (CSCs) (5). Ces¦dernières, définies comme étant une petite sous-population de cellules malignes, jouent un¦rôle prépondérant dans l'initiation et la progression tumorale. Elles partagent certaines¦propriétés avec les cellules souches physiologiques, telles que la capacité d'autorenouvellement,¦un potentiel de prolifération indéfini, une dépendance à un¦microenvironnement spécifique, une faculté de pluripotence et une résistance accrue aux¦drogues (6). Ce modèle de CSCs a également été étudié pour le NB (7), permettant ainsi¦d'avancer l'hypothèse selon laquelle cette population de CSCs serait responsable de la¦résistance aux chimiothérapies des cellules tumorales du NB.¦Afin de tenter d'éclaircir le caractère résistant aux drogues des CSCs du NB, nous avons¦sélectionné des sous-populations cellulaires résistantes, en traitant par divers agents¦cytotoxiques (cisplatine, doxorubicine, rapamycine et vincristine) cinq lignées différentes de¦neuroblastes. Dans le but d'établir un potentiel enrichissement en CSCs au sein de ces¦sous-populations par rapport aux populations contrôles non traitées, nous avons testé leurs¦fonctions d'auto-renouvellement et de clonogénicité. Ces propriétés ont été respectivement¦mises en évidence par la capacité des cellules à former des sphères de plusieurs¦générations dans des conditions de culture inhibant l'adhésion cellulaire et par la mesure de¦la croissance cellulaire en milieu semi-solide (soft agar assay). Une analyse d'expression¦génique effectuée préalablement par microarray (Human Genome U133Plus 2.0 Affymetrix¦GeneChip oligonucleotide) dans le laboratoire avait révélé une liste de gènes surexprimés¦dans les CSCs, dont fait partie mdr1 (8). Ce gène code la protéine de transport Pgp (Pglycoprotein),¦impliquée dans le mécanisme de résistance (9,10). Une étude par cytométrie¦en flux de l'expression de MDR1 dans nos diverses populations a également été réalisée¦afin de mettre en évidence une potentielle surexpression de ce gène au sein des cellules¦résistantes aux chimiothérapies

Circumstellar interaction of the type Ia supernova 2002ic

We propose a model to account for the bolometric light curve, quasi-continuum and the Ca II emission features of the peculiar type Ia supernova (SN) 2002ic, which exploded in a dense circumstellar envelope. The model suggests that the SN Ia had the maximum possible kinetic energy and that the ejecta expand in an approximately spherically symmetric (possibly clumpy) circumstellar environment. The Ca II and quasi-continuum are emitted by shocked SN ejecta that underwent deformation and fragmentation in the intershock layer. Modeling of the Ca II triplet implies that the contribution of the O I 8446 A line is about 25% of the 8500 A feature on day 234, which permits us to recover the flux in the Ca II 8579 A triplet from the flux of 8500 A blend reported by Deng et al. (2004). We use the Ca II doublet and triplet fluxes on day 234 to derive the electron temperature (~4400 K) in the Ca II line-emitting zone and the ratio of the total area of dense fragments to the area of the shell, S/S_0 ~ 100. We argue that Ca II bands and quasi-continuum originate from different zones of the shocked ejecta that reflect the abundance stratification of the supernova.Comment: 12 pages, MNRAS, in pres

Assessment of the chemosensitizing activity of TAT-RasGAP317-326 in childhood cancers.

Although current anti-cancer protocols are reasonably effective, treatment-associated long-term side effects, induced by lack of specificity of the anti-cancer procedures, remain a challenging problem in pediatric oncology. TAT-RasGAP317-326 is a RasGAP-derived cell-permeable peptide that acts as a sensitizer to various anti-cancer treatments in adult tumor cells. In the present study, we assessed the effect of TAT-RasGAP317-326 in several childhood cancer cell lines. The RasGAP-derived peptide-induced cell death was analyzed in several neuroblastoma, Ewing sarcoma and leukemia cell lines (as well as in normal lymphocytes). Cell death was evaluated using flow cytometry methods in the absence or in the presence of the peptide in combination with various genotoxins used in the clinics (4-hydroperoxycyclophosphamide, etoposide, vincristine and doxorubicin). All tested pediatric tumors, in response to at least one genotoxin, were sensitized by TAT-RasGAP317-326. The RasGAP-derived peptide did not increase cell death of normal lymphocytes, alone or in combination with the majority of the tested chemotherapies. Consequently, TAT-RasGAP317-326 may benefit children with tumors by increasing the efficacy of anti-cancer therapies notably by allowing reductions in anti-cancer drug dosage and the associated drug-induced side effects

Diffusive foam wetting process in microgravity

We report the experimental study of aqueous foam wetting in microgravity. The liquid fraction $\ell$ along the bubble edges is measured and is found to be a relevant dynamical parameter during the capillary process. The penetration of the liquid in the foam, the foam inflation, and the rigidity loss are shown all to obey strict diffusion processes.Comment: 4 pages, 6 figures, submitted to Phys. Rev. Let

Gamma-Ray Burst Environments and Progenitors

Likely progenitors for the GRBs (gamma-ray bursts) are the mergers of compact objects or the explosions of massive stars. These two cases have distinctive environments for the GRB afterglow: the compact object explosions occur in the ISM (interstellar medium) and those of massive stars occur in the preburst stellar wind. We calculate the expected afterglow for a burst in a Wolf-Rayet star wind and compare the results to those for constant, interstellar density. The optical afterglow for the wind case is generally expected to decline more steeply than in the constant density case, but this effect may be masked by variations in electron spectral index, and the two cases have the same evolution in the cooling regime. Observations of the concurrent radio and optical/X-ray evolution are especially useful for distinguishing between the two cases. The different rates of decline of the optical and X-ray afterglows of GRB 990123 suggest constant density interaction for this case. We have previously found strong evidence for wind interaction in SN 1998bw/GRB 980425 and here present a wind model for GRB 980519. We thus suggest that there are both wind type GRB afterglows with massive star progenitors and ISM type afterglows with compact binary star progenitors. The wind type bursts are likely to be accompanied by a supernova, but not the ISM type.Comment: 11 pages, 1 figure, revised version, ApJ Letters, in pres

Chandra Observations of SN 2004et and the X-ray Emission of Type IIp Supernovae

We report the X-ray detection of the Type II-plateau supernova SN 2004et in the spiral galaxy NGC 6946, using the Chandra X-Ray Observatory. The position of the X-ray source was found to agree with the optical position within ~0.4 arcsec. Chandra also surveyed the region before the 2004 event, finding no X-ray emission at the location of the progenitor. For the post-explosion observations, a total of 202, 151, and 158 photons were detected in three pointings, each ~29 ks in length, on 2004 October 22, November 6, and December 3, respectively. The spectrum of the first observation is best fit by a thermal model with a temperature of kT=1.3 keV and a line-of-sight absorption of N_H=1.0 x 10^{22} cm^{-2}. The inferred unabsorbed luminosity (0.4-8 keV) is ~4x10^{38} erg/s, adopting a distance of 5.5 Mpc. A comparison between hard and soft counts on the first and third epochs indicates a softening over this time, although there is an insufficient number of photons to constrain the variation of temperature and absorption by spectral fitting. We model the emission as arising from the reverse shock region in the interaction between the supernova ejecta and the progenitor wind. For a Type IIP supernova with an extended progenitor, the cool shell formed at the time of shock wave breakout from the star can affect the initial evolution of the interaction shell and the absorption of radiation from the reverse shock. The observed spectral softening might be due to decreasing shell absorption. We find a pre-supernova mass loss rate of (2-2.5)x 10^{-6} M_{\odot} /yr for a wind velocity of 10 kms, which is in line with expectations for a Type IIP supernova.Comment: total 19 pages including 7 figures. ApJ, in press. See http://spider.ipac.caltech.edu/staff/rho/preprint/SN2004etms.ps for the paper including full resolution image

Correlated Timing and Spectral Variations of the Soft X-ray Transient Aquila X-1: Evidence for an Atoll classification

Based on Rossi X-ray Timing Explorer data, we discuss the classification of the soft X-ray transient Aquila X-1 in the Z/atoll scheme, and the relation of its kilohertz quasi-periodic oscillations (kHz QPO) properties to the X-ray colors. The color-color diagram shows one elongated ("banana") structure and several "islands" of data points. The power spectra of the island are best represented by a broken power-law, whereas those of the banana by a power-law below ~ 1 Hz plus an exponentially cut-off component at intermediate frequencies (30-60 Hz). The parameters of these two components change in correlation with the position of the source in the color-color diagram. Based on the pattern that the source shows in the color-color diagram and its aperiodic variability we conclude that Aquila X-1 is an atoll source. We have also investigated the possible correlation between the frequency of the kHz QPO and the position of the source in the color-color diagram. The complexity seen in the frequency versus count rate diagram is reduced to a single track when the frequency is plotted against hard or soft color.Comment: 9 pages, 5 figures. Accepted for publication in Ap