bluuebunny/crossref_metadata_2025_split huggingface dataset:
J-PAS : Low-resolution (R ∼ 50) spectroscopy covering 8000 deg2
Authors: López-Sanjuan C. , Cenarro A. J. , Díaz-García L. A. , Muniesa D. J. , Roman I. San , Varela J. , Viironen K. ,   the J-PAS collaboration
Published: February 2015

AbstractWe present the ambitious project J-PAS, that will cover 8000 deg2 of the northern sky with 54 narrow-band (∼145Å) contiguous filters, all of them in the optical range (3700Å-9200Å). J-PAS will provide a low resolution spectra (R ∼ 50) in every pixel of the northern sky by 2020, leading to excellent photometric redshifts (0.3% uncertainty) of 100 million sources. J-PAS will permit the study of the 2D properties of nearby galaxies with unprecedented statistics. Some viable studies are the distribution of the star formation rate traced by Hα, the stellar populations gradients in elliptical galaxies up to a few effective radii, or the impact of environment in galaxy properties. In summary, J-PAS will bring a superb data set for 3D analysis in the local Universe.
Ionized gas outflows and global kinematics of low-z luminous star-forming galaxies
Authors: Arribas S. , Colina L. , Bellocchi E. , Maiolino R. , Villar-Martín M. 
Published: February 2015

AbstractWe have studied the kinematic properties of the ionized gas outflows and ambient interstellar medium (ISM) in a large and representative sample of local U/LIRGs (58 systems, 75 galaxies) at galactic and sub-galactic (i.e.,star-forming clumps) scales, thanks to integral field spectroscopy (IFS)-based high signal-to-noise integrated spectra. The main results have been recently presented in Arribas et al. (2014), and are briefly summarized here.
IFUs surveys, a panoramic view of galaxy evolution
Authors: Sánchez Sebastián F. ,   The CALIFA collaboration
Published: February 2015

AbstractWe present here a brief summary of the currenly on-going IFU surveys of galaxies in teh Local Universe, describing their main characteristics, including their sample selections, instrumental setups, wavelength ranges, and area of the galaxies covered. Finally, we make an emphasis on the main characteristics of the CALIFA survey and the more recent results that has been recently published.
The Scaling of Star Formation: from Molecular Clouds to Galaxies
Authors: Calzetti Daniela 
Published: February 2015

AbstractThis is a review of the extant literature and recent work on the scaling relation(s) that link the gas content of galaxies to the measured star formation rates. A diverse array of observing techniques and underlying physical assumptions characterize the determination of these relations at different scales, that range from the tens of parsec sizes of molecular clouds to the tens of kpc sizes of whole galaxies. Different techniques and measurements, and a variety of strategies, have been used by many authors to compare the scaling relations, both within and across galaxies. Although the picture is far from final, the past decade has seen tremendous progress in this field, and more progress is expected over the next several years.
Disk Galaxies in the Magneticum Pathfinder Simulations
Authors: Remus Rhea-Silvia , Dolag Klaus , Bachmann Lisa K. , Beck Alexander M. , Burkert Andreas , Hirschmann Michaela , Teklu Adelheid 
Published: February 2015

AbstractWe presentMagneticum Pathfinder, a new set of hydrodynamical cosmological simulations covering a large range of cosmological scales. Among the important physical processes included in the simulations are the chemical and thermodynamical evolution of the diffuse gas as well as the evolution of stars and black holes and the corresponding feedback channels. In the high resolution boxes aimed at studies of galaxy formation and evolution, populations of both disk and spheroidal galaxies are self-consistently reproduced. These galaxy populations match the observed stellar mass function and show the same trends for disks and spheroids in the mass–size relation as observations from the SDSS. Additionally, we demonstrate that the simulated galaxies successfully reproduce the observed specific angular-momentum–mass relations for the two different morphological types of galaxies. In summary, theMagneticum Pathfindersimulations are a valuable tool for studying the assembly of cosmic and galactic structures in the universe.
S7 : Probing the physics of Seyfert Galaxies through their ENLR & HII Regions
Authors: Dopita Michael A. , Shastri Prajval , Scharwächter Julia , Kewley Lisa J. , Davies Rebecca , Sutherland Ralph , Kharb Preeti , Jose Jessy , Bhatt Harish , Ramya S. , Hampton Elise , Jin Chichuan , Banfield Julie , Zaw Ingyin , Srivastava Shweta , James Bethan 
Published: February 2015

AbstractHere we present the first results from the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) which aims to investigate the physics of ∼140 radio-detected southern active Galaxies with z<0.02 through Integral Field Spectroscopy using the Wide Field Spectrograph (WiFeS). This instrument provides data cubes of the central 38×25 arc sec. of the target galaxies in the waveband 340–710nm with the unusually high resolution of R=7000 in the red (530–710nm), and R=3000 in the blue (340–560nm). These data provide the morphology, kinematics and the excitation structure of the extended narrow-line region, probe relationships with the black hole characteristics and the host galaxy, measures host galaxy abundance gradients and the determination of nuclear abundances from the HII regions. From photoionisation modelling, we may determine the shape of the ionising spectrum of the AGN, discover whether AGN metallicities differ from nuclear abundances determined from HII regions, and probe grain destruction in the vicinity of the AGN. Here we present some preliminary results and modelling of both Seyfert galaxies observed as part of the survey.
Dissecting galactic winds with the SAMI Galaxy Survey
Authors: Ho I-Ting ,   the SAMI Galaxy Survey Team
Published: February 2015

AbstractWe conduct a case study on a normal star-forming galaxy (z=0.05) observed by the SAMI Galaxy Survey and demonstrate the feasibility and potential of using large integral field spectroscopic surveys to investigate the prevalence of galactic-scale outflows in the local Universe. We perform spectral decomposition to separate the different kinematic components overlapping in the line-of-sight direction that causes the skewed line profiles in the integral field data. The three kinematic components present distinctly different line ratios and kinematic properties. We model the line ratios with the shock/photoionization code mappings iv and demonstrate that the different emission line properties are caused by major galactic outflows that introduce shock excitation in addition to photoionization. These results set a benchmark of the type of analysis that can be achieved by the SAMI Galaxy Survey on large numbers of galaxies.
Abundant molecular gas and inefficient SF in intra-cluster regions of a ram pressure stripped tail
Authors: Jáchym P. , Sun M. , Combes F. , Cortese L. , Kenney J. D. P. 
Published: February 2015

AbstractFor the first time in any ram pressure stripped galaxy, we detect large amounts of cold molecular gas in the X-ray bright, and star forming tail of ESO 137-001 in the Norma cluster. We find very low star formation efficiency in the stripped gas, similar to values found in the outer spiral disks where however molecular gas is mostly undetected. The results were recently published in Jáchym et al. (2014).
Oxygen abundances of zCOSMOS galaxies at z ∼ 1.4 based on five lines and implications for the fundamental metallicity relation
Authors: Maier Christian , Lilly Simon J. , Ziegler Bodo L. ,   zCOSMOS team
Published: February 2015

AbstractA relation between the stellar mass M and the gas-phase metallicity Z of galaxies, the MZR, is observed up to higher redshifts. It is a matter of debate, however, if the SFR is a second parameter in the MZR. To explore this issue at z > 1, we used VLT-SINFONI near-infrared (NIR) spectroscopy of eight zCOSMOS galaxies at 1.3 < z < 1.4 to measure the strengths of four emission lines: Hβ, [OIII]λ5007, Hα, and [NII]λ6584, additional to [OII]λ3727 measured from VIMOS. We derive reliable O/H metallicities based on five lines, and also SFRs from extinction corrected Hα measurements. We find that the MZR of these star-forming galaxies at z ≈ 1.4 is lower than the local SDSS MZR by a factor of three to five, a larger change than reported in the literature using [NII]/Hα-based metallicities from individual and stacked spectra. Correcting N2-based O/Hs using recent results by Newman et al. (2014), also the larger FMOS sample at z ∼ 1.4 of Zahid et al. (2014) shows a similar evolution of the MZR like the zCOSMOS objects. These observations seem also in agreement with a non-evolving FMR using the physically motivated formulation of the FMR from Lilly et al. (2013).
Jansky VLA S-band view of Hα emitters (HAEs) associated with a protocluster 4C23.56 at z = 2.5
Authors: Lee Minju , Suzuki Kenta , Kohno Kotaro , Tamura Yoichi , Iono Daisuke , Hatsukade Bunyo , Nakanishi Kouichiro , Tanaka Ichi , Kodama Tadayuki , Tadaki Kenichi , Ikarashi Soh , Ueda Junko , Umehata Hideki , Saito Toshiki , Kawabe Ryohei 
Published: February 2015

AbstractWe present recent results on Karl Jansky Very Large Array (JVLA) deep S-band (2-4 GHz) observation towards a protocluster 4C23.56 at redshift z ∼ 2.5. The protocluster 4C23.56 is known to have a significant over density (∼ 5 times) of star-burst galaxies selected to be Hα line-bright by a Subaru narrow band imaging. Now we have found 25 HAEs associated with the protocluster. These starburst HAEs are likely to become massive ellipticals at z = 0 in a cluster. Various other galaxy populations also reside in this field and the fact makes the field very unique as a tool to understand galaxy formation in a over dense region. Subsequent deep 1100-μm continuum surveys by the ASTE 10-m dish have discovered that several submillimeter bright galaxies (SMGs) coincide with HAEs, suggesting HAEs undergoing dusty starbursts. As star formation rates (SFRs) of HAEs might have been underestimated, we use radio being resistant to dust extinction. We investigate the correlation between SFR1.4 GHz and SFRHα for radio index α = 0.8 to see if the correlation holds for the sources and to check the number of dusty star forming galaxies. Our final results will allow us to evaluate quantitatively how the galaxy formation channel may be different under the condition of over-densities.
The relation between the gas, dust and total mass in edge-on spiral galaxies
Authors: Allaert Flor 
Published: February 2015

AbstractEach component of a galaxy plays its own unique role in regulating the galaxy's evolution. In order to understand how galaxies form and evolve, it is therefore crucial to study the distribution and properties of each of the various components, and the links between them, both radially and vertically. The latter is only possible in edge-on systems. We present the HEROES project, which aims to investigate the 3D structure of the interstellar gas, dust, stars and dark matter in a sample of 7 massive early-type spiral galaxies based on a multi-wavelength data set including optical, NIR, FIR and radio data.
The Structure and Kinematics of the ISM in Simulated Star-forming Galaxies
Authors: Baba Junichi , Morokuma-Matsui Kana , Saitoh Takayuki R. 
Published: February 2015

AbstractWe performed 3D N-body/hydrodynamic simulations of local and high-z (z ∼ 2) star-forming galaxies (SFGs) to investigate the structure and kinematic properties of the different ISM phases (i.e., ionized, atomic, and molecular gases). We took into account, for the first time, a fully non-equilibrium radiative cooling by solving the non-equilibrium chemistries of atoms (H, He, C and O) and molecules (H2 and CO), as well as radiative heating, star formation, heating by HII region and supernova explosions.
High-resolution, 3D radiative transfer modeling of M51
Authors: De Looze Ilse , Fritz Jacopo , Baes Maarten ,   Sag-2 consortium
Published: February 2015

AbstractWe present a new technique developed to model the radiative transfer (RT) effects in nearby face-on galaxies. The face-on perspective provides insight into the star-forming regions and clumpy structure, imposing the need for high-resolution 3D models to recover the asymmetric stellar and dust geometries observed in galaxies. RT modeling of the continuum emission of stars and its interaction with the embedding dust in a galaxy's interstellar medium enables a self-consistent study of the main dust heating mechanisms in galaxies. The main advantage of RT calculations is the non-local character of dust heating that can be addressed by tracing the propagation of stellar radiation through the dusty galaxy medium.
The formation and build-up of the red-sequence over the past 9 Gyr in VIPERS
Authors: Fritz Alexander ,   the VIPERS Team
Published: February 2015

AbstractWe present the Luminosity Function (LF) and Colour-Magnitude Relation (CMR) using ∼45000 galaxies drawn from the VIMOS Public Extragalactic Redshift Survey (VIPERS). Using different selection criteria, we define several samples of early-type galaxies and explore their impact on the evolution of the red-sequence (RS) and the effects of dust. Our results suggest a rapid build-up of the RS within a short time scale. We find a rise in the number density of early-type galaxies and a strong evolution in LF and CMR. Massive galaxies exist already 9 Gyr ago and experience an efficient quenching of their star formation at z = 1, followed by a passive evolution with only limited merging activity. In contrast, low-mass galaxies indicate a different mass assembly history and cause a slow build-up of the CMR over cosmic time.
Spatially resolved stellar populations with SAMI
Authors: Scott Nicholas ,   the SAMI team
Published: February 2015

AbstractUsing data from the SAMI Galaxy Survey we measure azimuthally averaged stellar age and metallicity profiles for ∼ 500 galaxies, using both luminosity-weighted Lick indices and mass-weighted full spectral fitting. We find a weak trend for steeper (i.e. more negative) metallicity gradients in more massive galaxies, however, below stellar masses ∼ 1010.5 M⊙, the scatter in metallicity gradient increases dramatically.
Environmental dependence of galaxy formation explored by near-infrared spectroscopy of two protoclusters at z>2
Authors: Shimakawa Rhythm , Kodama Tadayuki , Tadaki Ken-ichi , Hayashi Masao , Koyama Yusei , Tanaka Ichi 
Published: February 2015

AbstractProtoclusters at high redshifts are the ideal laboratories to study how the environmental dependences of galaxy properties seen in local Universe were initially set up when the progenitors of present-day early-type galaxies were in their early formation phases. We have conducted a deep near-infrared spectroscopy of Hα emitters (HAEs) associated with two protoclusters (PKS 1138–262 at z = 2.16 and USS 1558–003 at z = 2.53) with the Multi-Object Infrared Camera and Spectrograph (MOIRCS) on the Subaru telescope.As a result, the cluster membership of 27 and 36 HAEs are newly confirmed in these two protoclusters, respectively. The inferred dynamical masses of the protocluster cores are consistent with being the typical progenitors of present-day most massive clusters (Shimakawa et al.2014a). Also, those HAEs in the protoclusters show much higher [OIII]/Hβ ratios than local star forming galaxies. It is probably caused by the combination of their much higher specific star formation rates, lower gaseous metallicities and redshift evolution of inter-stellar medium. We also find that the mass-metallicity relation in the protocluster galaxies is offset to higher metallicity compared to those of field galaxies at a given stellar mass at M∗<1011M⊙ (Shimakawa et al.2014b). This trend is compatible with the recent work (Kulas et al.2013). The mass-metallicity relation is regulated not only by star formation history hence metal production history, but also by inflow and outflow processes that are known to be very active at z > 2 (Steide et al.2010). It suggests that the higher gaseous metallicities of protocluster galaxies may be caused by those gas transfer processes that are dependent on surrounding environments.
3D Study Of Magnetic Fields In NGC 6946
Authors: Williams Anna , Heald George , Wilcots Eric , Zweibel Ellen 
Published: February 2015

AbstractRecent advancements in both radio observatories and computing have opened a new regime of 3D observations. Not only do these instruments measure emission lines and radio continuum over much larger bandpasses, but they also simultaneously observe the polarized emission over the same large bandpasses with increased sensitivity. This “polarization spectrum" can be used to recover information about the 3D structure of magnetic fields in the universe. Our combined 3-20~cm observations of NGC 6946 taken with the Westerbork Synthesis Radio Telescope provide highly sensitive diagnostics of the internal depolarization across the galaxy. We use model fitting to determine likely mechanisms for depolarization in different regions of the galaxy, and glean information about the coherent and turbulent magnetic fields in NGC 6946. We produce Faraday dispersion maps that illustrate how we can probe different depths into the galaxy at different wavelengths and display new features of the line of sight magnetic field. This work is just a sample of the new 3D studies that are possible with upgraded and new radio instruments like the VLA, ATCA, and SKA.
Three-Dimensional Spectroscopy and Star Formation Histories of Field E+A Galaxies
Authors: Liu Charles T. , Wolf Marsha , Hooper Eric J. , Bather Joshua 
Published: February 2015

AbstractWe present the initial results of an integral field spectroscopic survey of E+A galaxies in the field, which combined with radio continuum measurements and multi-wavelength photometry and imaging provides significant insight into the dynamical and star formation histories of these transitioning post-starburst systems. We focus on the E+A galaxy known as G515 (z = 0.088), a massive merger remnant that began its star formation quenching process ∼ 1.0 Gyr ago. Its relatively young stellar population contrasts with its light profile and kinematics, which are more consistent with a slowly-rotating, early-type galaxy.
Incentivising improvements in health care delivery: a response to Adam Oliver
Authors: Doran Tim 
Published: February 2015

AbstractFinancial and reputational incentives are increasingly common components in strategies to performance manage the medical profession. Judging the impacts of incentives is challenging, however, and the science of framework design remains in its infancy. Oliver’s taxonomy therefore offers a useful and timely guide to the approaches that are most likely to be successful (and unsuccessful) in the field of health care. The use of incentives to date has focused on process measures and a narrow range of outcomes, a pragmatic approach that has produced some substantial quality gains within the constraints of existing health care systems. Improvement of specific technical aspects of quality may, however, have been achieved at the expense of trust, cooperation and benevolence. Deficits in these indispensible virtues will undermine any attempt to performance manage the medical and allied professions.
The role of the payment vehicle in non-market valuations of a health care service: willingness-to-pay for an ambulance helicopter service
Authors: Gyrd-Hansen Dorte 
Published: February 2015

AbstractThis study analyses the role of the payment vehicle when conducting non-market valuations of health care services using stated preference methods. Based on a contingent valuation study conducted in Denmark encompassing more than 3400 respondents three important conclusions are drawn. Firstly, it is found that the valuation of a publicly financed ambulance helicopter service is higher than for an identical privately financed service. Secondly, the results suggest that the public premium is likely to be partly driven by altruistic preferences, and that some citizens value access to this type of service for all. An important driver is also perceptions of quality of services across the private and public sector. Finally, it is shown that exclusion of protest bidders is problematic and may bias welfare estimates. The take home message is that it is difficult to isolate the value of a good per se, and that analysts should take care in applying the payment vehicle that is likely to be applied in real life when valuing non-market goods. There has been little awareness of the importance of choice of payment vehicle in the literature to date.
Cellular memory of hypoxia elicits neuroblastoma metastasis and enables invasion by non-aggressive neighbouring cells
Authors: Herrmann A , Rice M , Lévy R , Pizer B L , Losty P D , Moss D , Sée V 
Published: February 2015

AbstractTherapies targeting cancer metastasis are challenging owing to the complexity of the metastatic process and the high number of effectors involved. Although tumour hypoxia has previously been associated with increased aggressiveness as well as resistance to radio- and chemotherapy, the understanding of a direct link between the level and duration of hypoxia and the individual steps involved in metastasis is still missing. Using live imaging in a chick embryo model, we have demonstrated that the exposure of neuroblastoma cells to 1% oxygen for 3 days was capable of (1) enabling cell migration towards blood vessels, (2) slowing down their velocity within blood vessels to facilitate extravasation and (3) promoting cell proliferation in primary and secondary sites. We have shown that cells do not have to be hypoxic anymore to exhibit these acquired capabilities as a long-term memory of prior hypoxic exposure is kept. Furthermore, non-hypoxic cells can be influenced by neighbouring hypoxic preconditioned cells and be entrained in the metastatic progression. The acquired aggressive phenotype relies on hypoxia-inducible factor (HIF)-dependent transcription of a number of genes involved in metastasis and can be impaired by HIF inhibition. Altogether, our results demonstrate the need to consider both temporal and spatial tumour heterogeneity because cells can 'remember' an earlier environment and share their acquired phenotype with their close neighbours. As a consequence, it is necessary to monitor the correct hypoxic markers to be able to predict the consequences of the cells’ history on their behaviour and their potential response to therapies.