Concomitant chemotherapy (CT)–radiotherapy (RT) is a standard of care in locally advanced nasopharyngeal carcinoma (NPC) and a role for induction CT is not established.
Patients with locally advanced ...NPC, WHO type 2 or 3, were randomized to induction TPF plus concomitant cisplatin-RT or concomitant cisplatin-RT alone. The TPF regimen consisted of three cycles of Docetaxel 75mg/m2 day 1; cisplatin 75mg/m2 day 1; 5FU 750mg/m2/day days 1–5. RT consisted of 70Gy in 7weeks plus concomitant cisplatin 40mg/m2 weekly.
A total of 83 patients were included in the study. Demographics and tumour characteristics were well balanced between both arms. Most of the patients (95%) in the TPF arm received three cycles of induction CT. The rate of grade 3–4 toxicity and the compliance (NCI-CTCAE v3) during cisplatin-RT were not different between both arms. With a median follow-up of 43.1months, the 3-year PFS rate was 73.9% in the TPF arm versus 57.2% in the reference arm hazard ratio (HR)=0.44; 95% confidence interval (CI): 0.20–0.97, P=0.042. Similarly the 3years overall survival rate was 86.3% in the TPF arm versus 68.9% in the reference arm (HR=0.40; 95% CI: 0.15–1.04, P=0.05).
In conclusion, several important aspects can be emphasized: the compliance to induction TPF was good and TPF did not compromise the tolerance of the concomitant RT-cisplatin phase. The improved PFS and overall survival rates needs to be confirmed by further trials.
We present the detection of an unresolved radio source coincident with the position of the Type I superluminous supernova (SLSN) PTF10hgi (z = 0.098) about 7.5 yr post-explosion, with a flux density ...of F (6 GHz) 47.3 Jy and a luminosity of L (6 GHz) 1.1 × 1028 erg s−1 Hz−1. This represents the first detection of radio emission coincident with an SLSN on any timescale. We investigate various scenarios for the origin of the radio emission: star formation activity, an active galactic nucleus, and a non-relativistic supernova blastwave. While any of these would be quite novel if confirmed, none appear likely when considered within the context of the other properties of the host galaxy, previous radio observations of SLSNe, and the general population of hydrogen-poor supernovae (SNe). Instead, the radio emission is reminiscent of the quiescent radio source associated with the repeating FRB 121102, which has been argued to be powered by a magnetar born in a SLSN or long gamma-ray burst explosion several decades ago. We show that the properties of the radio source are consistent with a magnetar wind nebula or an off-axis jet, indicating the presence of a central engine. Our directed search for fast radio bursts from the location of PTF10hgi using 40 minutes of Very Large Array phased-array data reveals no detections to a limit of 22 mJy (10 ; 10 ms duration). We outline several follow-up observations that can conclusively establish the origin of the radio emission.
On 2019 April 25.346 and 26.640 UT the Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo gravitational-wave (GW) observatory announced the detection of the first candidate events ...in Observing Run 3 that contained at least one neutron star (NS). S190425z is a likely binary neutron star (BNS) merger at dL = 156 41 Mpc, while S190426c is possibly the first NS-black hole (BH) merger ever detected, at dL = 377 100 Mpc, although with marginal statistical significance. Here we report our optical follow-up observations for both events using the MMT 6.5 m telescope, as well as our spectroscopic follow-up of candidate counterparts (which turned out to be unrelated) with the 4.1 m SOAR telescope. We compare to publicly reported searches, explore the overall areal coverage and depth, and evaluate those in relation to the optical/near-infrared (NIR) kilonova emission from the BNS merger GW170817, to theoretical kilonova models, and to short gamma-ray burst (SGRB) afterglows. We find that for a GW170817-like kilonova, the partial volume covered spans up to about 40% for S190425z and 60% for S190426c. For an on-axis jet typical of SGRBs, the search effective volume is larger, but such a configuration is expected in at most a few percent of mergers. We further find that wide-field γ-ray and X-ray limits rule out luminous on-axis SGRBs, for a large fraction of the localization regions, although these searches are not sufficiently deep in the context of the γ-ray emission from GW170817 or off-axis SGRB afterglows. The results indicate that some optical follow-up searches are sufficiently deep for counterpart identification to about 300 Mpc, but that localizations better than 1000 deg2 are likely essential.
The discovery of a repeating fast radio burst (FRB) has led to the first precise localization, an association with a dwarf galaxy, and the identification of a coincident persistent radio source. ...However, further localizations are required to determine the nature of FRBs, the sources powering them, and the possibility of multiple populations. Here we investigate the use of associated persistent radio sources to establish FRB counterparts, taking into account the localization area and the source flux density. Due to the lower areal number density of radio sources compared to faint optical sources, robust associations can be achieved for less precise localizations as compared to direct optical host galaxy associations. For generally larger localizations that preclude robust associations, the number of candidate hosts can be reduced based on the ratio of radio-to-optical brightness. We find that confident associations with sources having a flux density of ∼0.01-1 mJy, comparable to the luminosity of the persistent source associated with FRB 121102 over the redshift range z 0.1-1, require FRB localizations of 20″. We demonstrate that even in the absence of a robust association, constraints can be placed on the luminosity of an associated radio source as a function of localization and dispersion measure (DM). For DM 1000 pc cm−3, an upper limit comparable to the luminosity of the FRB 121102 persistent source can be placed if the localization is 10″. We apply our analysis to the case of the ASKAP FRB 170107, using optical and radio observations of the localization region. We identify two candidate hosts based on a radio-to-optical brightness ratio of 100. We find that if one of these is indeed associated with FRB 170107, the resulting radio luminosity (1029− 4 × 1030 erg s−1 Hz−1, as constrained from the DM value) is comparable to the luminosity of the FRB 121102 persistent source.
On 2019 August 14 the Laser Interferometer Gravitational Wave Observatory (LIGO) and the Virgo gravitational wave interferometer announced the detection of a binary merger, S190814bv, with a low ...false alarm rate of about 1 in 1.6 × 1025 yr, a distance of 267 52 Mpc, a 90% (50%) localization region of about 23 (5) deg2, and a probability of being a neutron star-black hole (NS-BH) merger of >99%. The LIGO/Virgo Collaboration (LVC) defines NS-BH such that the lighter binary member has a mass of <3 M and the more massive one has >5 M , and this classification is in principle consistent with a BH-BH merger depending on the actual upper mass cutoff for neutron stars. Additionally, the LVC designated a probability that the merger led to matter outside the final BH remnant of <1%, suggesting that an electromagnetic (EM) counterpart is unlikely. Here we report our optical follow-up observations of S190814bv using the Magellan Baade 6.5 m telescope to target all 96 galaxies in the Galaxy List for the Advanced Detector Era catalog within the 50% localization volume (representing about 70% of the integrated luminosity within this region). No counterpart was identified to a median 3 limiting magnitude of i = 22.2 (Mi −14.9 mag), comparable to the brightness of the optical counterpart of the binary neutron star merger GW170817 at the distance of S190814bv; similarly, we can rule out an on-axis jet typical of short GRBs. However, we cannot rule out other realistic models, such as a kilonova with only ∼0.01 M of lanthanide-rich material, or an off-axis jet with a viewing angle of θobs 15°.
ABSTRACT We present photometry and spectroscopy of PS1-14bj, a hydrogen-poor superluminous supernova (SLSN) at redshift z = 0.5215 discovered in the last months of the Pan-STARRS1 Medium Deep Survey. ...PS1-14bj stands out because of its extremely slow evolution, with an observed rise of rest-frame days, and exponential decline out to ∼250 days past peak at a measured rate of , consistent with fully trapped 56Co decay. This is the longest rise time measured in an SLSN to date, and the first SLSN to show a rise time consistent with pair-instability supernova (PISN) models. Compared to other slowly evolving SLSNe, it is spectroscopically similar to the prototype SN 2007bi at maximum light, although lower in luminosity ( ) and with a flatter peak than previous events. PS1-14bj shows a number of peculiar properties, including a near-constant color temperature for days past peak, and strong emission lines from O iii λ5007 and O iii λ4363 with a velocity width of ∼3400 km s−1 in its late-time spectra. These both suggest there is a sustained source of heating over very long timescales, and are incompatible with a simple 56Ni-powered/PISN interpretation. A modified magnetar model including emission leakage at late times can reproduce the light curve, in which case the blue continuum and O iii features are interpreted as material heated and ionized by the inner pulsar wind nebula becoming visible at late times. Alternatively, the late-time heating could be due to interaction with a shell of H-poor circumstellar material.
We present optical observations of the Type I superluminous supernova (SLSN-I) SN 2017dwh at z 0.13, which reached Mi −21 mag at peak. Spectra taken a few days after peak show an unusual and strong ...absorption line centered near 3200 that we identify with Co ii, suggesting a high fraction of synthesized 56Ni in the ejecta. By ∼1 month after peak, SN 2017dwh became much redder than other SLSNe-I, instead strongly resembling broad-lined Type Ic supernovae (Ic-BL SNe) with clear suppression of the flux redward of ∼5000 , providing further evidence for a high mass of Fe-group elements. Late-time upper limits indicate a 56Ni mass of 0.6 M , leaving open the possibility that SN 2017dwh produced a 56Ni mass comparable to SN 1998bw ( 0.4 M ). Fitting the light curve with a combined magnetar and 56Ni model using MOSFiT, we find that the light curve can easily accommodate such masses without affecting the inferred magnetar parameters. We also find that SN 2017dwh occurred in the least-luminous detected host galaxy to date for an SLSN-I, with MB = −13.5 mag and an implied metallicity of Z ∼ 0.08 Z . The spectral properties of SN 2017dwh provide new evidence linking SLSNe-I with Type Ic-BL SNe, and in particular, the high Fe-group abundance may be due to enhanced 56Ni production or mixing due to asphericity. Finally, we find that SN 2017dwh represents the most extreme end of a correlation between continuum shape and Co ii absorption strength in the near-peak spectra of SLSNe-I, indicating that Fe-group abundance likely accounts for some of the variation in their spectral shapes.
Abstract Background Burnout syndrome occurs frequently amongst oncology healthcare workers. It has a detrimental effect on the patient–physician relationship. Little is known about the prevalence and ...causes of burnout amongst junior doctors in oncology. Methods An anonymous questionnaire was sent out to every medical or radiation oncology or haematology resident in France ( n = 340). It included: demographical data, burnout level (Maslach Burnout Inventory), sources of stress, sense of equity at work, sources of support, and general health questions. Validated scales were used when available. Two reminder e-mails were sent to increase the response rate. Results Questionnaires were despatched during Spring 2009. The response rate was 60% (204/340). Emotional exhaustion (EE) and Depersonalisation (DP), the major components of burnout, were reported, respectively, by 26% ( n = 53) and 35% ( n = 72) of the residents. Burnout prevalence was 44% ( n = 89), defined as a severely abnormal level of either EE or DP. Eighteen percent of the residents ( n = 36) had severely abnormal levels of both EE and DP. The burnout level was not significantly different between the three specialties, but was higher amongst residents who do not feel adequately rewarded for their work ( p < 0.001). Burnout was associated with a lower perception of one’s general health status ( p < 0.001) and the desire to quit Medicine or to change specialty ( p < 0.001). Conclusion The burnout level is high amongst oncology residents. It probably discourages vocations for oncology. Interventions are needed and could include support groups, more intense coaching by senior physicians, training programmes on ‘breaking bad news’ and teaching of stress management skills.
We show high resolution measurements of a surface plasmon resonance (SPR) sensor based on a rectangular nanohole array in a metal film. This SPR setup uses balanced intensity detection between two ...orthogonal polarizations of a He-Ne laser beam, which allows for sensitivity improvement, noise reduction and rejection of any uncorrelated variation in the intensity signal. A bulk sensitivity resolution of 6.4 x 10(-6) RIU is demonstrated. The proposed methodology is promising for applications in portable nanoplasmonic multisensing and imaging.
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