pinecone/core-2020-05-10-deduplication huggingface dataset:
Early type galaxies and structural parameters from ESO public survey
  KiDS

The Kilo Degree survey (KiDS) is a large-scale optical imaging survey carried
out with the VLT Survey Telescope (VST), which is the ideal tool for galaxy
evolution studies. We expect to observe millions of galaxies for which we
extract the structural parameters in four wavebands (u, g, r and i). This
sample will represent the largest dataset with measured structural parameters
up to a redshift $z=0.5$. In this paper we will introduce the sample, and
describe the 2D fitting procedure using the 2DPHOT environment and the
validation of the parameters with an external catalog.Comment: 4 pages, 2 figures, to appear on the refereed Proceeding of the "The
  Universe of Digital Sky Surveys" conference held at the INAF--OAC, Naples, on
  25th-28th november 2014, to be published on Astrophysics and Space Science
  Proceedings, edited by Longo, Napolitano, Marconi, Paolillo, Iodic
Searching for galaxy clusters in the VST-KiDS Survey

We present the methods and first results of the search for galaxy clusters in
the Kilo Degree Survey (KiDS). The adopted algorithm and the criterium for
selecting the member galaxies are illustrated. Here we report the preliminary
results obtained over a small area (7 sq. degrees), and the comparison of our
cluster candidates with those found in the RedMapper and SZ Planck catalogues;
the analysis to a larger area (148 sq. degrees) is currently in progress. By
the KiDS cluster search, we expect to increase the completeness of the clusters
catalogue to z = 0.6-0.7 compared to RedMapper.Comment: 5 pages, 4 figures, to be published in the Proceedings of the
  Conference "The Universe of Digital Sky Surveys", Naples, November 25-28 201
The Wide Area VISTA Extra-galactic Survey (WAVES)

The "Wide Area VISTA Extra-galactic Survey" (WAVES) is a 4MOST Consortium
Design Reference Survey which will use the VISTA/4MOST facility to
spectroscopically survey ~2million galaxies to $r_{\rm AB} < 22$ mag. WAVES
consists of two interlocking galaxy surveys ("WAVES-Deep" and "WAVES-Wide"),
providing the next two steps beyond the highly successful 1M galaxy Sloan
Digital Sky Survey and the 250k Galaxy And Mass Assembly survey. WAVES will
enable an unprecedented study of the distribution and evolution of mass,
energy, and structures extending from 1-kpc dwarf galaxies in the local void to
the morphologies of 200-Mpc filaments at $z\sim1$. A key aim of both surveys
will be to compare comprehensive empirical observations of the spatial
properties of galaxies, groups, and filaments, against state-of-the-art
numerical simulations to distinguish between various Dark Matter models.Comment: Refereed Proceeding of the "The Universe of Digital Sky Surveys"
  conference held at the INAF - Observatory of Capodimonte, Naples, on
  25th-28th november 2014, to be published on Astrophysics and Space Science
  Proceedings, edited by Longo, Napolitano, Marconi, Paolillo, Iodic
Systematic variation of central mass density slope in early-type
  galaxies

We study the total density distribution in the central regions ($<\, 1$
effective radius, $R_{\rm e}$) of early-type galaxies (ETGs), using data from
the SPIDER survey. We model each galaxy with two components (dark matter halo +
stars), exploring different assumptions for the dark matter (DM) halo profile,
and leaving stellar mass-to-light ($M_{\rm \star}/L$) ratios as free fitting
parameters to the data. For a Navarro et al. (1996) profile, the slope of the
total mass profile is non-universal. For the most massive and largest ETGs, the
profile is isothermal in the central regions ($\sim R_{\rm e}/2$), while for
the low-mass and smallest systems, the profile is steeper than isothermal, with
slopes similar to those for a constant-M/L profile. For a concentration-mass
relation steeper than that expected from simulations, the correlation of
density slope with mass tends to flatten. Our results clearly point to a
"non-homology" in the total mass distribution of ETGs, which simulations of
galaxy formation suggest may be related to a varying role of dissipation with
galaxy mass.Comment: 3 pages, 1 figure, to appear on the refereed Proceeding of the "The
  Universe of Digital Sky Surveys" conference held at the INAF--OAC, Naples, on
  25th-28th november 2014, to be published on Astrophysics and Space Science
  Proceedings, edited by Longo, Napolitano, Marconi, Paolillo, Iodic
Luminosity functions in the CLASH-VLT cluster MACS J1206.2-0847: the
  importance of tidal interactions

We present the optical luminosity functions (LFs) of galaxies for the
CLASH-VLT cluster MACS J1206.2-0847 at z=0.439, based on HST and SUBARU data,
including ~600 spectroscopically confirmed member galaxies. The LFs on the wide
SUBARU FoV are well described by a single Schechter function down to M~M*+3,
whereas this fit is poor for HST data, due to a faint-end upturn visible down
M~M*+7, suggesting a bimodal behaviour. We also investigate the effect of local
environment by deriving the LFs in four different regions, according to the
distance from the centre, finding an increase in the faint-end slope going from
the core to the outer rings. Our results confirm and extend our previous
findings on the analysis of mass functions, which showed that the galaxies with
stellar mass below 10^10.5, M_sun have been significantly affected by tidal
interaction effects, thus contributing to the intra cluster light.Comment: 5 pages, 2 figures, Proceeding of the talk at the conference "The
  Universe of Digital Sky Surveys" held in Naples (Italy) on 25-28 November
  201
A Semi-automatic Search for Giant Radio Galaxy Candidates and their
  Radio-Optical Follow-up

We present results of a search for giant radio galaxies (GRGs) with a
projected largest linear size in excess of 1 Mpc. We designed a computational
algorithm to identify contiguous emission regions, large and elongated enough
to serve as GRG candidates, and applied it to the entire 1.4-GHz NRAO VLA Sky
survey (NVSS). In a subsequent visual inspection of 1000 such regions we
discovered 15 new GRGs, as well as many other candidate GRGs, some of them
previously reported, for which no redshift was known. Our follow-up
spectroscopy of 25 of the brighter hosts using two 2.1-m telescopes in Mexico,
and four fainter hosts with the 10.4-m Gran Telescopio Canarias (GTC), yielded
another 24 GRGs. We also obtained higher-resolution radio images with the Karl
G. Jansky Very Large Array for GRG candidates with inconclusive radio
structures in NVSS.Comment: 4 pages, 1 figure, to appear in the proceedings of The Universe of
  Digital Sky Surveys, Naples, Italy, Nov 25-28, 2014; Astrophysics and Space
  Science, eds. N.R. Napolitano et a
The WiFeS S7 AGN survey: Current status and recent results on NGC 6300

The Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) is a
targeted survey probing the narrow-line regions (NLRs) of a representative
sample of ~140 nearby (z<0.02) Seyfert galaxies by means of optical integral
field spectroscopy. The survey is based on a homogeneous data set observed
using the Wide Field Spectrograph WiFeS. The data provide a 25x38 arcsec$^2$
field-of-view around the galaxy centre at typically ~1.5 arcsec spatial
resolution and cover a wavelength range between ~3400 - 7100 $\AA$ at spectral
resolutions of ~100 km s$^{-1}$ and ~50 km s$^{-1}$ in the blue and red parts,
respectively. The survey is primarily designed to study gas excitation and star
formation around AGN, with a special focus on the shape of the AGN ionising
continuum, the interaction between radio jets and the NLR gas, and the nature
of nuclear LINER emission. We provide an overview of the current status of
S7-based results and present new results for NGC 6300.Comment: 5 pages, 1 figure, Refereed Proceeding of the "The Universe of
  Digital Sky Surveys" conference held at the INAF - Observatory of
  Capodimonte, Naples, on 25th-28th november 2014, to be published on
  Astrophysics and Space Science Proceedings, edited by Longo, Napolitano,
  Marconi, Paolillo, Iodic
A new search for variability-selected active galaxies within the VST
  SUDARE-VOICE survey: the Chandra Deep Field South and the SERVS-SWIRE area

This work makes use of the VST observations to select variable sources. We
use also the IR photometry, SED fitting and X-ray information where available
to confirm the nature of the AGN candidates. The IR data, available over the
full survey area, allow to confirm the consistency of the variability selection
with the IR color selection method, while the detection of variability may
prove useful to detect the presence of an AGN in IR selected starburst
galaxies.Comment: Refereed Proceeding of the "The Universe of Digital Sky Surveys"
  conference held at the INAF - Observatory of Capodimonte, Naples, on
  25th-28th november 2014, to be published on Astrophysics and Space Science
  Proceedings, edited by Longo, Napolitano, Marconi, Paolillo, Iodic
An overview of the EXTraS project: Exploring the X-ray Transient and
  Variable Sky

The EXTraS project (Exploring the X-ray Transient and variable Sky) will
harvest the hitherto unexplored temporal domain information buried in the
serendipitous data collected by the European Photon Imaging Camera (EPIC)
instrument onboard the ESA XMM-Newton X-ray observatory since its launch. This
will include a search for fast transients, as well as a search and
characterization of variability (both periodic and aperiodic) in hundreds of
thousands of sources spanning more than nine orders of magnitude in time scale
and six orders of magnitude in flux. X-ray results will be complemented by
multiwavelength characterization of new discoveries. Phenomenological
classification of variable sources will also be performed. All our results will
be made available to the community. A didactic program in selected High Schools
in Italy, Germany and the UK will also be implemented. The EXTraS project
(2014-2016), funded within the EU/FP7 framework, is carried out by a
collaboration including INAF (Italy), IUSS (Italy), CNR/IMATI (Italy),
University of Leicester (UK), MPE (Germany) and ECAP (Germany).Comment: 6 pages, 1 figure. Proceedings of "Swift: 10 years of Discovery", to
  appear in Po
Galactic Plane H$\alpha$ Surveys: IPHAS & VPHAS+

The optical Galactic Plane H$\alpha$ surveys IPHAS and VPHAS+ are
dramatically improving our understanding of Galactic stellar populations and
stellar evolution by providing large samples of stars in short lived, but
important, evolutionary phases, and high quality homogeneous photometry and
images over the entire Galactic Plane. Here I summarise some of the
contributions these surveys have already made to our understanding of a number
of key areas of stellar and Galactic astronomy.Comment: 5 pages, 2 figures, refereed proceeding of the "The Universe of
  Digital Sky Surveys" conference, November 2014, to be published in the
  Astrophysics and Space Science Proceeding
Stellar Streams and Clouds in the Galactic Halo

Recent years have seen the discovery of an ever growing number of stellar
debris streams and clouds. These structures are typically detected as extended
and often curvilinear overdensities of metal-poor stars that stand out from the
foreground disk population. The streams typically stretch tens of degrees or
more across the sky, even encircling the Galaxy, and range in heliocentric
distance from 3 to 100 kpc. This chapter summarizes the techniques used for
finding such streams and provides tables giving positions, distances,
velocities, and metallicities, where available, for all major streams and
clouds that have been detected as of January 2015. Sky maps of the streams are
also provided. Properties of individual tidal debris structures are discussed.Comment: 27 pages, 6 figures, Book chapter in Tidal Streams in the Local Group
  and Beyond, eds. Heidi Newberg and Jeff Carli
Kinematically Detected Halo Streams

Clues to the origins and evolution of our Galaxy can be found in the
kinematics of stars around us. Remnants of accreted satellite galaxies produce
over- densities in velocity-space, which can remain coherent for much longer
than spatial over-densities. This chapter reviews a number of studies that have
hunted for these accretion relics, both in the nearby solar-neighborhood and
the more-distant stellar halo. Many observational surveys have driven this
field forwards, from early work with the Hipparcos mission, to contemporary
surveys like RAVE & SDSS. This active field continues to flourish, providing
many new discoveries, and will be revolutionised as the Gaia mission delivers
precise proper motions for a billion stars in our Galaxy.Comment: 27 pages, 10 figures. Chapter from Springer ASSL Volume entitled
  "Tidal Streams in the Local Group and Beyond". Affluent readers may wish to
  purchase the full volume here:
  http://link.springer.com/book/10.1007/978-3-319-19336-
Origins and Interpretation of Tidal Debris

The stellar debris structures that have been discovered around the Milky Way
and other galaxies are thought to be formed from the disruption of satellite
stellar systems --- dwarf galaxies or globular clusters --- by galactic tidal
fields. The total stellar mass in these structures is typically tiny compared
to the galaxy around which they are found, and it is hence easy to dismiss them
as inconsequential. However, they are remarkably useful as probes of a galaxy's
history (as described in this chapter) and mass distribution (covered in a
companion chapter in this volume). This power is actually a consequence of
their apparent insignificance: their low contribution to the overall mass makes
the physics that describes them both elegant and simple and this means that
their observed properties are relatively easy to understand and interpret.Comment: Chapter~6 from the volume "Tidal Streams in the Local Group and
  Beyond: Observations and Implications"; ed. Newberg, H.~J., \& Carlin, J.~L.\
  2016, Springer International Publishing, Astrophysics and Space Science
  Library, 420\\ ISBN 978-3-319-19335-9; DOI 10.1007/978-3-319-19336-6\_
Tidal Debris as a Dark Matter Probe

Tidal debris streams from galaxy satellites can provide insight into the dark
matter distribution in halos. This is because we have more information about
stars in a debris structure than about a purely random population of stars: we
know that in the past they were all bound to the same dwarf galaxy; and we know
that they form a dynamically cold population moving on similar orbits. They
also probe a different region of the matter distribution in a galaxy than many
other methods of mass determination, as their orbits take them far beyond the
typical extent of those for the bulk of stars. Although conclusive results from
this information have yet to be obtained, significant progress has been made in
developing the methodologies for determining both the global mass distribution
of the Milky Way's dark matter halo and the amount of dark matter substructure
within it. Methods for measuring the halo shape are divided into "predictive
methods," which predict the tidal debris properties from the progenitor
satellite's mass and orbit, given an assumed parent galaxy mass distribution;
and "fundamental methods," which exploit properties fundamental to the nature
of tidal debris as global potential constraints. Methods for quantifying the
prevalence of dark matter subhalos within halos through the analysis of the
gaps left in tidal streams after these substructures pass through them are
reviewed.Comment: Chapter~7 from the volume "Tidal Streams in the Local Group and
  Beyond: Observations and Implications"; ed. Newberg, H.~J., \& Carlin, J.~L.\
  2016, Spr inger International Publishing, Astrophysics and Space Science
  Library, 420\\ IS BN 978-3-319-19335-9; DOI 10.1007/978-3-319-19336-6\_
Substructure and Tidal Streams in the Andromeda Galaxy and its
  Satellites

Tidal streams from existing and destroyed satellite galaxies populate the
outer regions of the Andromeda galaxy (M31). This inhomogeneous debris can be
studied without many of the obstacles that plague Milky Way research. We review
the history of tidal stream research in M31, and in its main satellite
galaxies. We highlight the numerous tidal streams observed around M31, some of
which reside at projected distances of up to 120 kpc from the center of this
galaxy. Most notable is the Giant Stellar Stream, a signature of the most
recent significant accretion event in the M31 system. This event involved an
early-type progenitor of ~10^9 solar masses that came within a few kpc of M31's
center roughly a gigayear ago; almost all of the inner halo debris (within 50
kpc) in M31 can be tied either directly or indirectly to this event. We draw
attention to the fact that most of M31's outer halo globular clusters lie
preferentially on tidal streams and discuss the potential this offers to use
these systems as probes of the accretion history. Tidal features observed
around M33, M32, NGC 205 and NGC 147 are also reviewed. We conclude by
discussing future prospects for this field.Comment: 29 pages, 9 figures. Book chapter in Tidal Streams in the Local Group
  and Beyond, eds. Heidi Newberg and Jeff Carli
Stellar Tidal Streams in External Galaxies

To place the highly substructured stellar halos of the Milky Way and M31 in a
larger context of hierarchical galaxy formation, it is necessary to understand
the prevalence and properties of tidal substructure around external galaxies.
This chapter details the current state of our observational knowledge of
streams in galaxies in and beyond the Local Group, which are studied both in
resolved stellar populations and in integrated light. Modeling of individual
streams in extragalactic systems is hampered by our inability to obtain
resolved stellar kinematics in the streams, though many streams contain
alternate luminous kinematic tracers, such as globular clusters or planetary
nebulae. We compare the observed structures to the predictions of models of
galactic halo formation, which provide insight in the number and properties of
streams expected around Milky Way like galaxies. More specifically, we discuss
the inferences that can be made about stream progenitors based only on observed
morphologies. We expand our discussion to consider hierarchical accretion at
lower mass scales, in particular the observational evidence that substructure
exists on smaller mass scales and the effects accretion events may have on the
evolution of dwarf galaxies (satellite or isolated). Lastly, we discuss
potential correlations between the presence of substructure in the halo and the
structural properties of the disk. While many exciting discoveries have been
made of tidal substructures around external galaxies, the "global" questions of
galaxy formation and evolution via hierarchical accretion await a more complete
census of the low surface brightness outskirts of galaxies in and beyond the
Local Group.Comment: 28 pages, 9 figures. Book chapter in Tidal Streams in the Local Group
  and Beyond, eds. Heidi Newberg and Jeff Carlin. Astrophysics and Space
  Science Library, Volume 420. ISBN 978-3-319-19335-9. Springer International
  Publishing Switzerland, 2016, p. 21
Towards a better understanding and behavior recognition of inhabitants
  in smart cities. A public transport case

The idea of modern urban systems and smart cities requires monitoring and
careful analysis of different signals. Such signals can originate from
different sources and one of the most promising is the BTS, i.e. base
transceiver station, an element of mobile carrier networks. This paper presents
the fundamental problems of elicitation, classification and understanding of
such signals so as to develop context-aware and pro-active systems in urban
areas. These systems are characterized by the omnipresence of computing which
is strongly focused on providing on-line support to users/inhabitants of smart
cities. A method of analyzing selected elements of mobile phone datasets
through understanding inhabitants' behavioral fingerprints to obtain smart
scenarios for public transport is proposed. Some scenarios are outlined. A
multi-agent system is proposed. A formalism based on graphs that allows
reasoning about inhabitant behaviors is also proposed.Comment: Proceedings of 14th International Conference on Arificial Inteligence
  and Soft Computing (ICAISC 2015), 14-18 June, 2015, Zakopane, Poland; Lecture
  Notes in Computer Science, vol. 9120, pp.237-246. Springer Verlag 201
Theoretical Models of the Galactic Bulge

Near infrared images from the COBE satellite presented the first clear
evidence that our Milky Way galaxy contains a boxy shaped bulge. Recent years
have witnessed a gradual paradigm shift in the formation and evolution of the
Galactic bulge. Bulges were commonly believed to form in the dynamical violence
of galaxy mergers. However, it has become increasingly clear that the main body
of the Milky Way bulge is not a classical bulge made by previous major mergers,
instead it appears to be a bar seen somewhat end-on. The Milky Way bar can form
naturally from a precursor disk and thicken vertically by the internal
firehose/buckling instability, giving rise to the boxy appearance. This picture
is supported by many lines of evidence, including the asymmetric parallelogram
shape, the strong cylindrical rotation (i.e., nearly constant rotation
regardless of the height above the disk plane), the existence of an intriguing
X-shaped structure in the bulge, and perhaps the metallicity gradients. We
review the major theoretical models and techniques to understand the Milky Way
bulge. Despite the progresses in recent theoretical attempts, a complete bulge
formation model that explains the full kinematics and metallicity distribution
is still not fully understood. Upcoming large surveys are expected to shed new
light on the formation history of the Galactic bulge.Comment: Invited review to appear in "Galactic Bulges", Editors: Laurikainen
  E., Peletier R., Gadotti D., Springer Publishing, 2015, in press. 27 pages, 7
  figure
Galaxy bulges and their massive black holes: a review

With references to both key and oft-forgotten pioneering works, this article
starts by presenting a review into how we came to believe in the existence of
massive black holes at the centres of galaxies. It then presents the historical
development of the near-linear (black hole)-(host spheroid) mass relation,
before explaining why this has recently been dramatically revised. Past
disagreement over the slope of the (black hole)-(velocity dispersion) relation
is also explained, and the discovery of sub-structure within the (black
hole)-(velocity dispersion) diagram is discussed. As the search for the
fundamental connection between massive black holes and their host galaxies
continues, the competing array of additional black hole mass scaling relations
for samples of predominantly inactive galaxies are presented.Comment: Invited (15 Feb. 2014) review article (submitted 16 Nov. 2014). 590
  references, 9 figures, 25 pages in emulateApJ format. To appear in "Galactic
  Bulges", E. Laurikainen, R.F. Peletier, and D.A. Gadotti (eds.), Springer
  Publishin