First author: J. Prat
Recent cosmological analyses with large-scale structure and weak lensing measurements, usually referred to as 3$\times$2pt, had to discard a lot of signal-to-noise from small scales due to our inability to precisely model non-linearities and baryonic effects. Galaxy-galaxy lensing, or the position-shear correlation between lens and source galaxies, is one of the three two-point correlation functions that are included in such analyses, usually estimated with the mean tangential shear.
Kuantay Boshkayev
We reproduce the rotation curve of the Andromeda galaxy (M31) by taking into account its bulge, disk, and halo components, considering the last one to contain the major part of dark matter mass. Hence, our prescription is to split the galactic bulge into two components, namely, the inner and main bulges, respectively. Both bulges are thus modeled by exponential density profiles since we underline that the widely accepted de Vaucouleurs law fails to reproduce the whole galactic bulge rotation curve.
First author: M. S. Rosito
The morphological classification of galaxies is considered a relevant issue and can be approached from different points of view. The increasing growth in the size and accuracy of astronomical data sets brings with it the need for the use of automatic methods to perform these classifications. The aim of this work is to propose and evaluate a method for automatic unsupervised classification of kinematic morphologies of galaxies that yields a meaningful clustering and captures the variations of the fundamental properties of galaxies.
First author: M. Sharma
We derive the Ultra-Violet (UV) luminosity function (LF) of star forming galaxies falling in the redshift range $z = 0.6 - 1.2$, in the rest-frame far-UV (1500 {\AA}) wavelength. For this work we are in particular interested in the bright end of the UV LF in this redshift range. The data from \textit{XMM-Newton} Optical Monitor (XMM-OM), near-ultraviolet (1600-4000 {\AA}) observations over 1.5 deg\textsuperscript{2} of the COSMOS field are employed for this purpose.
I. D. Karachentsev
The <span class="search-hit mathjax">dwarf</span> irregular <span class="search-hit mathjax">galaxy</span> HIPASS J1131-31 was discovered as a source of HI emission at low redshift in such close proximity of a bright star that we call it Peekaboo. The <span class="search-hit mathjax">galaxy</span> resolves into stars in images with Hubble Space Telescope, leading to a distance estimate of 6.8+-0.7 Mpc. Spectral optical observations with the Southern African Large Telescope reveal HIPASS J1131-31 to be one of the most extremely metal-poor <span class="search-hit mathjax">galaxies</span> known with the gas-phase oxygen abundance 12+log(O/H) = 6.
First author: I. D. Karachentsev
The dwarf irregular galaxy HIPASS J1131-31 was discovered as a source of HI emission at low redshift in such close proximity of a bright star that we call it Peekaboo. The galaxy resolves into stars in images with Hubble Space Telescope, leading to a distance estimate of 6.8+-0.7 Mpc. Spectral optical observations with the Southern African Large Telescope reveal HIPASS J1131-31 to be one of the most extremely metal-poor galaxies known with the gas-phase oxygen abundance 12+log(O/H) = 6.
Nils Hoyer
We use high-resolution Hubble Space Telescope imaging data of <span class="search-hit mathjax">dwarf</span> <span class="search-hit mathjax">galaxies</span> in the Local Volume ($\lesssim 11$ Mpc) to parameterise 19 newly discovered nuclear star clusters (NSCs). Most of the clusters have stellar masses of $M_{\star}^{nsc} \lesssim 10^6$ M$_{\odot}$ and compare to Galactic globular clusters in terms of ellipticity, effective radius, stellar mass, and surface density. The clusters are modelled with a Sérsic profile and their surface brightness evaluated at the effective radius reveals a tight positive correlation to the host <span class="search-hit mathjax">galaxy</span> stellar mass.
First author: Nils Hoyer
We use high-resolution Hubble Space Telescope imaging data of dwarf galaxies in the Local Volume ($\lesssim 11$ Mpc) to parameterise 19 newly discovered nuclear star clusters (NSCs). Most of the clusters have stellar masses of $M_{\star}^{nsc} \lesssim 10^6$ M${\odot}$ and compare to Galactic globular clusters in terms of ellipticity, effective radius, stellar mass, and surface density. The clusters are modelled with a S'ersic profile and their surface brightness evaluated at the effective radius reveals a tight positive correlation to the host galaxy stellar mass.
First author: Dennis Zaritsky
We present a photometric halo mass estimation technique for local galaxies that enables us to establish the stellar mass-halo mass (SMHM) relation down to stellar masses of 10$^5$ M$\odot$. We find no detectable differences among the SMHM relations of four local galaxy clusters or between the cluster and field relations and we find agreement with extrapolations of previous SMHM relations derived using abundance matching approaches. We fit a power law to our empirical SMHM relation and find that for adopted NFW dark matter profiles and for M$* < 10^9$ M$\odot$, the halo mass is M$h = 10^{10.
First author: O. Petruk
The detected polarized radio emission from remnant of SN1987A opens the possibility to unveil the structure of the pre-supernova magnetic field in the circumstellar medium. Properties derived from direct measurements would be of importance for understanding the progenitor stars and their magnetic fields. As the first step to this goal, we adopted the hydrodynamic data from an elaborated three-dimensional (3-D) numerical model of SN1987A. We have developed an approximate method for reconstruction' of 3-D magnetic field structure inside supernova remnant on the hydrodynamic background’.
