We present high time resolution (1.09 s) photometry of GRB 080210 obtained with ULTRASPEC mounted on the ESO/3.6-m telescope, starting 68.22 min after the burst and lasting for 26.45 min. The light ...curve is smooth on both short (down to 2.18 s) and long time scales, confirmed by a featureless power spectrum. On top of the fireball power-law decay, bumps and wiggles at different time scales can, in principle, be produced by density fluctuations in the circumburst medium, by substructures in the jet or by refreshed shocks. Comparing our constraints with variability limits derived from kinematic arguments, we exclude under-density fluctuations producing flux dips larger than 1 per cent with time scales Δt > 9.2 min (2 per cent on Δt > 2.3 min for many fluctuating regions). In addition, we study the VLT/FORS2 afterglow spectrum, the optical-to-X-ray spectral energy distribution (SED) and the time decay. The SED is best fitted with a broken power law with slopes βopt= 0.71 ± 0.01 and βX= 1.59 ± 0.07, in disagreement with the fireball model, suggesting a non-standard afterglow for GRB 080210. We find AV
= 0.18 ± 0.03 mag optical extinction due to SMC-like dust and an excess X-ray absorption of log(N
H/cm−2) = 21.58+0.18
−0.26 assuming solar abundances. The spectral analysis reveals a damped Lyα absorber (log
cm−2) = 21.90 ± 0.10) with a low metallicity (X/H=−1.21 ± 0.16), likely associated with the interstellar medium of the GRB host galaxy (z= 2.641).
Background and purpose To identify the beneficial effects of primary stroke centers (PSCs) certification by Joint Commission (JC), we compared the rates of in-hospital adverse events and discharge ...outcomes among ischemic stroke patients admitted to PSCs and those admitted to non-PSC hospitals in the United States. Methods We obtained the data from the Nationwide Inpatient Sample from 2010 and 2011. The analysis was limited to states that publicly reported hospital identity. PSCs were identified by matching the Nationwide Inpatient Sample hospital files with the list provided by JC. The analysis was limited to patients (age ≥18 years) discharged with a principal diagnosis of ischemic stroke (International Classification of Disease, 9th Revision, codes 433.x1, 434.x1). Results We identified a total of 123,131 ischemic stroke patients from 28 states. A total of 72,982 (59.3%) patients were admitted to PSCs. After adjusting for age, gender, race or ethnicity, comorbidities, All Patients Refined Diagnosis Related Groups (APR-DRG)-based disease severity, and hospital teaching status, patients admitted to PSCs were at lower risk of in-hospital adverse events complications: pneumonia (odds ratio OR, .8; 95% confidence interval CI, .7-.8) and sepsis (OR, .7; 95% CI, .6-.8). Patients admitted to PSCs were more likely to receive thrombolysis (OR, 1.6; 95% CI, 1.5-1.7). The mean cost of hospitalization (95% CI) of the patients was significantly higher in patients admitted at PSCs compared with those admitted at non PSC hospitals $47621 (47099-48144) vs. $35229 (34803-35654), P < .0001). The patients admitted to PSCs had lower inpatient mortality (OR, .8; 95% CI, .8-.9) and were more likely to be discharged with none to minimal disability (OR, 1.1; 95% CI, 1.0-1.1). Conclusions Compared with non-PSC admissions, patients admitted to PSCs are less likely to experience hospital adverse events and more likely to experience better discharge outcomes.
A scaling relation has recently been suggested to combine the galaxy mass–metallicity (MZ) relation with metallicities of damped Lyman α systems (DLAs) in quasar spectra. Based on this relation the ...stellar masses of the absorbing galaxies can be predicted. We test this prediction by measuring the stellar masses of 12 galaxies in confirmed DLA absorber–galaxy pairs in the redshift range 0.1 < z < 3.2. We find an excellent agreement between the predicted and measured stellar masses over three orders of magnitude, and we determine the average offset 〈C
M/H〉 = 0.44 ± 0.10 between absorption and emission metallicities. We further test if C
M/H could depend on the impact parameter and find a correlation at the 5.5σ level. The impact parameter dependence of the metallicity corresponds to an average metallicity difference of −0.022 ± 0.004 dex kpc−1. By including this metallicity versus impact parameter correlation in the prescription instead of C
M/H, the scatter reduces to 0.39 dex in log M
*. We provide a prescription on how to calculate the stellar mass (
$M_*^{\mathrm{DLA}}$
) of the galaxy when both the DLA metallicity and DLA galaxy impact parameter is known. We demonstrate that DLA galaxies follow the MZ relation for luminosity-selected galaxies at z = 0.7 and 2.2 when we include a correction for the correlation between impact parameter and metallicity.
Context. Short duration gamma-ray bursts (SGRBs) are thought to be related to the violent merger of compact objects, such as neutron stars or black holes, which makes them promising sources of ...gravitational waves. The detection of a “kilonova”-likesignature associated to the Swift-detected GRB 130603B has suggested that this event is the result of a compact object merger. Aims. Our knowledge on SGRB has been, until now, mostly based on the absence of supernova signatures and the analysis of the host galaxies to which they cannot always be securely associated. Further progress has been significantly hampered by the faintness and rapid fading of their optical counterparts (afterglows), which has so far precluded spectroscopy of such events. Afterglow spectroscopy is the key tool to firmly determine the distance at which the burst was produced, crucial to understand its physics, and study its local environment. Methods. Here we present the first spectra of a prototypical SGRB afterglow in which both absorption and emission features are clearly detected. Together with multi-wavelength photometry we study the host and environment of GRB 130603B. Results. From these spectra we determine the redshift of the burst to be z = 0.3565 ± 0.0002, measure rich dynamics both in absorption and emission, and a substantial line of sight extinction of AV = 0.86 ± 0.15 mag. The GRB was located at the edge of a disrupted arm of a moderately star forming galaxy with near-solar metallicity. Unlike for most long GRBs (LGRBs), NHX/AV is consistent with the Galactic ratio, indicating that the explosion site differs from those found in LGRBs. Conclusions. The merger is not associated with the most star-forming region of the galaxy; however, it did occur in a dense region, implying a rapid merger or a low natal kick velocity for the compact object binary.
Context. Q 0151+048 is a physical quasar (QSO) pair at z ~ 1.929 with a separation of 3.3 arcsec on the sky. In the spectrum of the brighter member of this pair, Q 0151+048A, a damped Lyα absorber ...(DLA) is observed at a higher redshift. We have previously detected the host galaxies of both QSOs, as well as a Lyα blob whose emission surrounding Q 0151+048A extends over 5 × 3.3 arcsec. Aims. We seek to constrain the geometry of the system and understand the possible relations between the DLA, the Lyα blob, and the two QSOs. We also aim at characterizing the former two objects in more detail. Methods. To study the nature of the Lyα blob, we performed low-resolution, long-slit spectroscopy with the slit aligned with the extended emission. We also observed the whole system using the medium-resolution VLT/X-shooter spectrograph and the slit aligned with the two QSOs. The systemic redshift of both QSOs was determined from rest-frame optical emission lines redshifted into the NIR. We employed line-profile fitting technique, to measure metallicities and the velocity width of low-ionization metal absorption lines associated to the DLA and photo-ionization modeling to characterize the DLA further. Results. We measure systemic redshifts of zem(A) = 1.92924 ± 0.00036 and zem(B) = 1.92863 ± 0.00042 from the H β and H α emission lines, respectively. In other words, the two QSOs have identical redshifts within 2σ. From the width of Balmer emission lines and the strength of the rest-frame optical continuum, we estimate the masses of the black holes of the two QSOs to be 109.33 M⊙ and 108.38 M⊙ for Q 0151+048A and Q 0151+048B, respectively. We then use the correlation between black hole mass and dark matter halo mass to infer the mass of the dark matter halos hosting the two QSOs: 1013.74 M⊙ and 1013.13 M⊙ for Q 0151+048A and Q 0151+048B, respectively. We observe a velocity gradient along the major axis of the Lyα blob consistent with the rotation curve of a large disk galaxy, but it may also be caused by gas inflow or outflow. We detect residual continuum in the DLA trough, which we interpret as emission from the host galaxy of Q 0151+048A. The derived H0 column density of the DLA is log NH0 = 20.34 ± 0.02 cm-2. Metal column densities are also determined for a number of low-ionization species resulting in an overall metallicity of 0.01 Z⊙. We detect C ii ∗ , which allows us to make a physical model of the DLA cloud. Conclusions. From the systemic redshifts of the QSOs, we conclude that the Lyα blob is associated with Q 0151+048A rather than with the DLA. The DLA must be located in front of both the Lyα blob and Q 0151+048A at a distance greater than 30 kpc and has a velocity relative to the blob of 640 ± 70 km s-1. The two quasars accrete at normal Eddington ratios. The DM halo of this double quasar will grow to the mass of our local supercluster at z = 0. We point out that those objects therefore form an ideal laboratory to study the physical interactions in a z = 2 precursor of our local supercluster.
We present here a dataset of quasars observed with the Ultraviolet Visual Echelle Spectrograph (UVES) on the Very Large Telescope and available in the European Southern Observatory UVES Advanced Data ...Products archive. The sample is made up of a total of 250 high resolution quasar spectra with emission redshifts ranging from 0.191 \textless= z(em) \textless= 6.311. The total UVES exposure time of this dataset is 1560 h. Thanks to the high resolution of UVES spectra, it is possible to unambiguously measure the column density of absorbers with damping wings, down to N-HI greater than or similar to 10(19) cm(-2), which constitutes the sub-damped Ly alpha absorber (sub-DLA) threshold. Within the wavelength coverage of our UVES data, we find 150 damped Lya systems (DLAs)/sub-DLAs in the range 1.5 \textless z(abs) \textless 4.7. Of these 150, 93 are DLAs and 57 are sub-DLAs. An extensive search in the literature indicates that 6 of these DLAs and 13 of these sub-DLAs have their N-HI measured for the first time. Among them, 10 are new identifications as DLAs/sub-DLAs. For each of these systems, we obtain an accurate measurement of the Hi column density and the absorber's redshift in the range 1.7 \textless z(abs) \textless 4.2 by implementing a Voigt profile-fitting algorithm. These absorbers are further confirmed thanks to the detection of associated metal lines and/or lines from members of the Lyman series. In our data, a few quasars' lines-of-sight are rich. An interesting example is towards QSO J0133+ 0400 (z(em) = 4.154) with six DLAs and sub-DLAs reported.
Advance care planning, including code/resuscitation status discussion, is an essential part of the medical care of patients with CKD. There is little information on the outcomes of cardiopulmonary ...resuscitation in these patients. We aimed to measure cardiopulmonary resuscitation outcomes in these patients.
Our study is observational in nature. We compared the following cardiopulmonary resuscitation-related outcomes in patients with CKD with those in the general population by using the Nationwide Inpatient Sample (2005-2011): (
) survival to hospital discharge, (
) discharge destination, and (
) length of hospital stay. All of the patients were 18 years old or older.
During the study period, 71,961 patients with CKD underwent in-hospital cardiopulmonary resuscitation compared with 323,620 patients from the general population. Unadjusted in-hospital mortality rates were higher in patients with CKD (75% versus 72%;
<0.001) on univariate analysis. After adjusting for age, sex, and potential confounders, patients with CKD had higher odds of mortality (odds ratio, 1.24; 95% confidence interval, 1.11 to 1.34;
≤0.001) and length of stay (odds ratio, 1.11; 95% confidence interval, 1.07 to 1.15;
=0.001). Hospitalization charges were also greater in patients with CKD. There was no overall difference in postcardiopulmonary resuscitation nursing home placement between the two groups. In a separate subanalysis of patients ≥75 years old with CKD, higher odds of in-hospital mortality were also seen in the patients with CKD (odds ratio, 1.10; 95% confidence interval, 1.02 to 1.17;
=0.01).
In conclusion, we observed slightly higher in-hospital mortality in patients with CKD undergoing in-hospital cardiopulmonary resuscitation.
Context. Absorbing galaxies are selected via the detection of characteristic absorption lines which their gas-rich media imprint in the spectra of distant light-beacons. The proximity of the ...typically faint foreground absorbing galaxies to bright background sources makes it challenging to robustly identify these in emission, and hence to characterise their relation to the general galaxy population. Aims. We search for emission to confirm and characterise ten galaxies hosting damped, metal-rich quasar absorbers at redshift z < 1. Methods. We identified the absorbing galaxies by matching spectroscopic absorption -and emission redshifts and from projected separations. Combining emission-line diagnostics with existing absorption spectroscopy and photometry of quasar-fields hosting metal-rich, damped absorbers, we compare our new detections with reference samples and place them on scaling relations. Results. We spectroscopically confirm seven galaxies harbouring damped absorbers (a 70% success-rate). Our results conform to the emerging picture that neutral gas on scales of tens of kpc in galaxies is what causes the characteristic H I absorption. Our key results are: (I) Absorbing galaxies with log10M⋆,(M⊙) ≳ 10 have star formation rates that are lower than predicted for the main sequence of star formation. (II) The distribution of impact parameter with H I column density and with absorption-metallicity for absorbing galaxies at z ∼ 2–3 extends to z ∼ 0.7 and to lower H I column densities. (III) A robust mean metallicity gradient of ⟨Γ⟩ = −0.022 ± 0.001 dex kpc−1. (IV) By correcting absorption metallicities for ⟨Γ⟩ and imposing a truncation-radius at 12 kpc, absorbing galaxies fall on top of predicted mass-metallicity relations, with a statistically significant decrease in scatter.
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