198 research outputs found
Targeted Radionuclide Therapy using high-LET particle emitter-labeled vectors against alpha-v-beta6-expressing cancers
Cosmological measurements from void-galaxy and galaxy-galaxy clustering in the Sloan Digital Sky Survey
We present the cosmological implications of measurements of void-galaxy and
galaxy-galaxy clustering from the Sloan Digital Sky Survey (SDSS) Main Galaxy
Sample (MGS), Baryon Oscillation Spectroscopic Survey (BOSS), and extended BOSS
(eBOSS) luminous red galaxy catalogues from SDSS Data Release 7, 12, and 16,
covering the redshift range . We fit a standard CDM
cosmological model as well as various extensions including a constant dark
energy equation of state not equal to , a time-varying dark energy equation
of state, and these same models allowing for spatial curvature. Results on key
parameters of these models are reported for void-galaxy and galaxy-galaxy
clustering alone, both of these combined, and all these combined with
measurements from the cosmic microwave background (CMB) and supernovae (SN).
For the combination of void-galaxy and galaxy-galaxy clustering plus CMB and
SN, we find tight constraints of for a
base CDM cosmology, additionally allowing the dark energy equation of state to
vary, and further extending to
non-flat models.Comment: 11 pages, 9 figures. Submitted to MNRA
Constraining CDM with density-split clustering
The dependence of galaxy clustering on local density provides an effective
method for extracting non-Gaussian information from galaxy surveys. The
two-point correlation function (2PCF) provides a complete statistical
description of a Gaussian density field. However, the late-time density field
becomes non-Gaussian due to non-linear gravitational evolution and higher-order
summary statistics are required to capture all of its cosmological information.
Using a Fisher formalism based on halo catalogues from the Quijote simulations,
we explore the possibility of retrieving this information using the
density-split clustering (DS) method, which combines clustering statistics from
regions of different environmental density. We show that DS provides more
precise constraints on the parameters of the CDM model compared to
the 2PCF, and we provide suggestions for where the extra information may come
from. DS improves the constraints on the sum of neutrino masses by a factor of
and by factors of 5, 3, 4, 6, and 6 for , , , ,
and , respectively. We compare DS statistics when the local density
environment is estimated from the real or redshift-space positions of haloes.
The inclusion of DS autocorrelation functions, in addition to the
cross-correlation functions between DS environments and haloes, recovers most
of the information that is lost when using the redshift-space halo positions to
estimate the environment. We discuss the possibility of constructing
simulation-based methods to model DS clustering statistics in different
scenarios.Comment: Submitted to MNRAS. Source code for all figures in the paper is
provided in the caption
175 Contribution of direct and bystander effects to therapeutic efficacy of alpha-RIT using 212Pb-labeled mAbs
SN 2009N: linking normal and subluminous Type II-P Sne
We present ultraviolet, optical, near-infrared photometry and spectroscopy of
SN 2009N in NGC 4487. This object is a type II-P supernova with spectra
resembling those of subluminous II-P supernovae, while its bolometric
luminosity is similar to that of the intermediate luminosity SN 2008in. We
created SYNOW models of the plateau phase spectra for line identification and
to measure the expansion velocity. In the near-infrared spectra we find signs
indicating possible weak interaction between the supernova ejecta and the
pre-existing circumstellar material. These signs are also present in the
previously unpublished near-infrared spectra of SN 2008in. The distance to SN
2009N is determined via the expanding photosphere method and the standard
candle method as . The produced nickel-mass
is estimated to be . We infer the
physical properties of the progenitor at the explosion through hydrodynamical
modelling of the observables. We find the values of the total energy as , the ejected mass as , and the initial radius as .Comment: 23 pages, 18 figures, accepted for publication by MNRA
SN 2009N: linking normal and subluminous Type II-P SNe
We present ultraviolet, optical, near-infrared photometry and spectroscopy of SN 2009N in NGC 4487. This object is a Type II-P supernova with spectra resembling those of subluminous II-P supernovae, while its bolometric luminosity is similar to that of the intermediate-luminosity SN 2008in. We created SYNOW models of the plateau phase spectra for line identification and to measure the expansion velocity. In the near-infrared spectra we find signs indicating possible weak interaction between the supernova ejecta and the pre-existing circumstellar material. These signs are also present in the previously unpublished near-infrared spectra of SN 2008in. The distance to SN 2009N is determined via the expanding photosphere method and the standard candle method as D = 21.6 +/- 1.1 Mpc. The produced nickel-mass is estimated to be similar to 0.020 +/- 0.004 M-circle dot. We infer the physical properties of the progenitor at the explosion through hydrodynamical modelling of the observables. We find the values ofthe total energy as similar to 0.48 x 10(51) erg, the ejected mass as similar to 11.5 M-circle dot, and the initial radius as similar to 287 R-circle dot.</p
SN 2011hs: a fast and faint Type IIb supernova from a supergiant progenitor
Observations spanning a large wavelength range, from X-ray to radio, of the Type IIb supernova (SN) 2011hs are presented, covering its evolution during the first year after explosion. The optical light curve presents a narrower shape and a fainter luminosity at peak than previously observed for Type IIb SNe. High expansion velocities are measured from the broad absorption H I and He I lines. From the comparison of the bolometric light curve and the time evolution of the photospheric velocities with hydrodynamical models, we found that SN 2011hs is consistent with the explosion of a 3–4 M⊙ He-core progenitor star, corresponding to a main-sequence mass of 12–15 M⊙, that ejected a mass of 56Ni of about 0.04 M⊙, with an energy of E = 8.5 × 1050 ERG. Such a low-mass progenitor scenario is in full agreement with the modelling of the nebular spectrum taken at ∼215 d from maximum. From the modelling of the adiabatic cooling phase, we infer a progenitor radius of ≈500–600 R⊙, clearly pointing to an extended progenitor star. The radio light curve of SN 2011hs yields a peak luminosity similar to that of SN 1993J, but with a higher mass-loss rate and a wind density possibly more similar to that of SN 2001ig. Although no significant deviations from a smooth decline have been found in the radio light curves, we cannot rule out the presence of a binary companion star
SN 2009ib: a Type II-P supernova with an unusually long plateau
We present optical and near-infrared photometry and spectroscopy of SN 2009ib, a Type II-P supernova in NGC 1559. This object has moderate brightness, similar to those of the intermediate-luminosit ..
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