14,669 research outputs found
The bivariate gas-stellar mass distributions and the mass functions of early- and late-type galaxies at
We report the bivariate HI- and H-stellar mass distributions of local
galaxies in addition of an inventory of galaxy mass functions, MFs, for HI,
H, cold gas, and baryonic mass, separately into early- and late-type
galaxies. The MFs are determined using the HI and H conditional
distributions and the galaxy stellar mass function, GSMF. For the conditional
distributions we use the compilation presented in Calette et al. 2018. For
determining the GSMF from to
, we combine two spectroscopic samples from the SDSS at the redshift
range . We find that the low-mass end slope of the GSMF, after
correcting from surface brightness incompleteness, is ,
consistent with previous determinations. The obtained HI MFs agree with radio
blind surveys. Similarly, the H MFs are consistent with CO follow-up
optically-selected samples. We estimate the impact of systematics due to
mass-to-light ratios and find that our MFs are robust against systematic
errors. We deconvolve our MFs from random errors to obtain the intrinsic MFs.
Using the MFs, we calculate cosmic density parameters of all the baryonic
components. Baryons locked inside galaxies represent 5.4% of the universal
baryon content, while % of the HI and H mass inside galaxies reside
in late-type morphologies. Our results imply cosmic depletion times of H
and total neutral H in late-type galaxies of and 7.2 Gyr,
respectively, which shows that late type galaxies are on average inefficient in
converting H into stars and in transforming HI gas into H. Our results
provide a fully self-consistent empirical description of galaxy demographics in
terms of the bivariate gas--stellar mass distribution and their projections,
the MFs. This description is ideal to compare and/or to constrain galaxy
formation models.Comment: 37 pages, 17 figures. Accepted for publication in PASA. A code that
displays tables and figures with all the relevant statistical distributions
and correlations discussed in this paper is available here
https://github.com/arcalette/Python-code-to-generate-Rodriguez-Puebla-2020-result
Stability of Influence Maximization
The present article serves as an erratum to our paper of the same title,
which was presented and published in the KDD 2014 conference. In that article,
we claimed falsely that the objective function defined in Section 1.4 is
non-monotone submodular. We are deeply indebted to Debmalya Mandal, Jean
Pouget-Abadie and Yaron Singer for bringing to our attention a counter-example
to that claim.
Subsequent to becoming aware of the counter-example, we have shown that the
objective function is in fact NP-hard to approximate to within a factor of
for any .
In an attempt to fix the record, the present article combines the problem
motivation, models, and experimental results sections from the original
incorrect article with the new hardness result. We would like readers to only
cite and use this version (which will remain an unpublished note) instead of
the incorrect conference version.Comment: Erratum of Paper "Stability of Influence Maximization" which was
presented and published in the KDD1
Collective resonances in plasmonic crystals: Size matters
Periodic arrays of metallic nanoparticles may sustain Surface Lattice
Resonances (SLRs), which are collective resonances associated with the
diffractive coupling of Localized Surface Plasmon Resonances (LSPRs). By
investigating a series of arrays with varying number of particles, we traced
the evolution of SLRs to its origins. Polarization resolved extinction spectra
of arrays formed by a few nanoparticles were measured, and found to be in very
good agreement with calculations based on a coupled dipole model. Finite size
effects on the optical properties of the arrays are observed, and our results
provide insight into the characteristic length scales for collective plasmonic
effects: for arrays smaller than 5 x 5 particles, the Q-factors of SLRs are
lower than those of LSPRs; for arrays larger than 20 x 20 particles, the
Q-factors of SLRs saturate at a much larger value than those of LSPRs; in
between, the Q-factors of SLRs are an increasing function of the number of
particles in the array.Comment: 4 figure
Nekrasov-Shatashvili limit of the 5D superconformal index
C. P. is supported by the Royal Society through a University Research Fellowship. A. P. and D. R. G. are partly supported by the Spanish Government Grant No. MINECO-13-FPA2012-35043-C02-02. In addition, they acknowledge financial support from the Ramon y Cajal Grant No. RYC-2011-07593 as well as the EU CIG Grant No. UE-14-GT5LD2013-618459. The work of A. P. is funded by the Asturian Government SEVERO OCHOA Grant No. BP14-003
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