bluuebunny/crossref_metadata_2025_split huggingface dataset:
Quenching of Star-formation Activity of High-redshift Galaxies in Clusters and Field
Authors: Lee Seong-Kook , Im Myungshin , Kim Jae-Woo , Lotz Jennifer , McPartland Conor , Peth Michael , Koekemoer Anton 
Published: August 2016

AbstractAt local, galaxy properties are well known to be clearly different in different environments. However, it is still an open question how this environment-dependent trend has been shaped. We present the results of our investigation about the evolution of star-formation properties of galaxies over a wide redshift range, from z ~ 2 to z ~ 0.5, focusing its dependence on their stellar mass and environment (Lee et al. 2015). In the UKIDSS/UDS region, covering ~2800 square arcmin, we estimated photometric redshifts and stellar population properties, such as stellar masses and star-formation rates, using the deep optical and near-infrared data available in this field. Then, we identified galaxy cluster candidates within the given redshift range. Through the analysis and comparison of star-formation (SF) properties of galaxies in clusters and in field, we found interesting results regarding the evolution of SF properties of galaxies: (1) regardless of redshifts, stellar mass is a key parameter controlling quenching of star formation in galaxies; (2) At z < 1, environmental effects become important at quenching star formation regardless of stellar mass of galaxies; and (3) However, the result of the environmental quenching is prominent only for low mass galaxies (M* < 1010 M⊙) since the star formation in most of high mass galaxies are already quenched at z > 1.
UV escape fraction and dust distribution of star forming galaxies at z = 0-3: a new dust attenuation model
Authors: Kusakabe Haruka , Shimasaku Kazuhiro , Shimizu Ikkoh 
Published: August 2016

AbstractThe UV escape fraction, fescUV, is a key parameter determining the apparent SED of star forming galaxies. However, it is not well known how fescUV depends on the global geometry of dust distribution, nor how it evolves with time, although several models are proposed (e.g., Calzetti (2001)). We use ~130 normal star-forming galaxies (114 at z ~ 0 from Cortese et al. (2012) and 15 at z ~ 1–3 from Magnelli et al. (2012) and Saintonge et al. (2013)), to find that the z ~ 0 galaxies show a relatively tight anti-correlation between fescUV and surface dust mass density, Σd (See Fig. 1(a)). This correlation can be reproduced by a dust geometry model that well-mixed stars and dust follow the same exponential profile (Fig. 1(b)) with an effective mass-absorption coefficient κ(1600 Å) = 7.6+5.3−3.0 × 104 cm2 g−1, similar to the Milky Way value including absorption and scatter. The z ~ 1–3 galaxies are not inconsistent with this model. Our model can be easily implemented in semi-analytic models and cosmological hydrodynamics simulations (CHSs) of galaxy formation. Initial results for Shimizu et al. (2014)'s CHSs are presented.
The High-Redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey
Authors: Paterno-Mahler Rachel , Blanton Elizabeth L. , Wing Joshua , Ashby M.L.N. , Brodwin Mark , Golden-Marx Emmet 
Published: August 2016

AbstractThe number of confirmed, high-redshift galaxy clusters is very low compared to the number of well-studied clusters nearby. Bent, double-lobed radio sources are frequently found in galaxy clusters, and thus can be used as tracers for efficiently locating high-redshift clusters. Using our Spitzer Snapshot Survey, we have identified approximately 300 potential new clusters with redshifts 0.7 < z < 3. These objects make up the high-redshift portion of the Cluster Occupied by Bent Radio AGN (COBRA) survey. We have created color-magnitude diagrams using infrared and optical data. Using the colors of the radio source host and the red sequence we can estimate redshifts for our clusters, as well as examine the evolution of the cluster galaxies over a large range of cosmic time.
High–redshift quasars and blazars and their relation to high–redshift galaxies
Authors: Mickaelian Areg , Abrahamyan Hayk , Paronyan Gurgen 
Published: August 2016

AbstractHigh–redshift quasars and blazars are among the most powerful sources in the Universe and among the highest luminosity sources, as in optical, so as in X–ray, UV, IR and radio range. We have created a full sample of blazars and high–redshift quasars (z≥2.15). The evolutionary relation of high–redshift quasars and blazars to high–redshift galaxies is discussed using the luminosity evolution.
Ultra Massive Passive Galaxies at z~1.7
Authors: Arcila-Osejo Liz , Sawicki Marcin , Golob Anneya , Arnouts Stephane , Moutard Thibaud 
Published: August 2016

AbstractAt redshift z~1.7 the Universe was at the peak of its star-formation activity. It is thus a puzzle why some galaxies, many of them very massive (M* ⩾ 1011 M⊙), had already chosen to stop forming stars. These ultra-massive galaxies, guaranteed to be the central galaxies of their host dark matter halos, must have attained very high rates of star formation to assemble their stellar masses in such a short amount of time. Using the largest (to date) K-selected gzKs survey of passive galaxies (in an effective area of ~ 27.5 deg2) we study the demographics of these dead monsters, hoping to help understand the quenching mechanism that shut them down.
A consistent view on star-forming galaxies at high redshift from multi-wavelength observations and SED modeling
Authors: Schaerer Daniel , de Barros Stephane , Boone Frederic 
Published: August 2016

AbstractWe stress the importance of consistent SED analysis for distant star-forming galaxies (SFGs). We then summarise recent results from such an analysis concerning their basic physical properties, such as the determination of star formation rate (SFR), stellar mass, specific star SFR, UV attenuation, and how this affects our knowledge of star formation properties at high-z.
SXDF-UDS-CANDELS-ALMA 1.5 arcmin2 deep survey
Authors: Kohno K. , Yamaguchi Y. , Tamura Y. , Tadaki K. , Hatsukade B. , Ikarashi S. , Caputi K.I. , Rujopakarn W. , Ivison R.J. , Dunlop J.S. , Motohara K. , Umehata H. , Yabe K. , Wang W.H. , Kodama T. , Koyama Y. , Hayashi M. , Matsuda Y. , Hughes D. , Aretxaga I. , Wilson G.W. , Yun M.S. , Ohta K. , Akiyama M. , Kawabe R. , Iono D. , Nakanishi K. , Lee M. , Makiya R. 
Published: August 2016

AbstractWe have conducted 1.1 mm ALMA observations of a contiguous 105” × 50” or 1.5 arcmin2 window in the SXDF-UDS-CANDELS. We achieved a 5σ sensitivity of 0.28 mJy, giving a flat sensus of dusty star-forming galaxies with LIR ~6×1011L⊙ (if Tdust=40K) up to z ~ 10 thanks to the negative K-correction at this wavelength. We detected 5 brightest sources (S/N>6) and 18 low-significant sources (5>S/N>4; they may contain spurious detections, though). One of the 5 brightest ALMA sources (S1.1mm = 0.84 ± 0.09 mJy) is extremely faint in the WFC3 and VLT/HAWK-I images, demonstrating that a contiguous ALMA imaging survey uncovers a faint dust-obscured population invisible in the deep optical/near-infrared surveys. We find a possible [CII]-line emitter at z=5.955 or a low-z CO emitting galaxy within the field, allowing us to constrain the [CII] and/or CO luminosity functions across the history of the universe.
SuperMassive Blackholes grow from stellar BHs of star formation history?
Authors: Rocca-Volmerange Brigitte 
Published: August 2016

AbstractThe origin of the supermassive black hole masses MSMBH discovered at the highest redshifts is still actively debated. Moreover the statistically significant relation of MSMBH with bulge luminosities LV, extended on several magnitude orders, confirms a common physical process linking small (≤ 1pc) to large (kpcs) size scales. The Spectral Energy Distributions (SEDs) of two z=3.8 radio galaxies 4C41.17 and TN J2007-1316, best-fitted by evolved early type galaxy and starburst scenarios also imply masses of stellar remnants. Computed with the evolutionary code Pegase.3, the cumulated stellar black hole mass MsBH reach up to several 109M⊙, similar to MSMBH at same z. We propose the SMBH growth is due to the migration of the stellar dense residues (sBH) towards the galaxy core by dynamical friction. Discussed in terms of time-scales, this process which is linking AGN and star formation, also fully justifies the famous relation MSMBH-LV.
Galaxies at z ~ 6: physical properties at the edge of the cosmic reionization
Authors: de Barros Stephane , Vanzella Eros , Pentericci Laura , Fontana Adriano , Grazian Andrea , Castellano Marco 
Published: August 2016

AbstractAn important effort has been recently made to detect spectroscopically galaxies at z ~ 6 and higher where the cosmic reionization is thought to occur. The drop of the fraction of Lyman Alpha Emitters (LAEs) at z>6 is currently interpreted as an effect of the increasing neutral hydrogen density.We present preliminary results from the latest VLT/FORS2 programs, combined with ESO archival data, to perform a large census of z ~ 6 galaxies. We derive their physical properties as stellar mass and dust attenuation with an SED fitting tool including nebular emission which is of primeval importance because IRAC channels are strongly contaminated by emission lines at those redshifts. We take a special care to derive with precision the redshift of non LAEs to perform a comparison of their properties with the LAE population and derive as accurately as possible the fraction of LAEs. In particular, we compare the UV beta slope with the Lyα equivalent width which are known to correlate at lower redshift.We also report the detection of few peculiar z ~ 6 galaxies with extremely blue UV β slope (~−3), which can be a signature of unusual stellar populations (e.g., very hot and massive stars).
The VIMOS Ultra Deep Survey: Lyα Emission and Stellar Populations of Star-Forming Galaxies at 2 < z < 6
Authors: Hathi Nimish P. , Le Fèvre Olivier ,   the VUDS team
Published: August 2016

AbstractThe extensive ground-based spectroscopy campaign from the VIMOS Ultra-Deep Survey (VUDS), and the deep multi-wavelength photometry in three very well observed extragalactic fields (ECDFS, COSMOS, VVDS), allow us to investigate physical properties of a large sample (~4000 galaxies) of spectroscopically confirmed faint (iAB ≲ 25 mag) SFGs, with and without Lyα in emission, at z ~ 2–6. The fraction of Lyα emitters (LAEs; equivalent width (EW) ≥ 20Å) increases from ~10% at z ~ 2 to ~40% at z ~ 5–6, which is consistent with previous studies that employ higher Lyα EW cut. This increase in the LAE fraction could be, in part, due to a decrease in the dust content of galaxies as redshift increases. When we compare best-fit SED estimated stellar parameters for LAEs and non-LAEs, we find that Es(B-V) is smaller for LAEs at all redshifts and the difference in the median Es(B-V) between LAEs and non-LAEs increases as redshift increases, from 0.05 at z ~ 2 to 0.1 at z ~ 3.5 to 0.2 at z ~ 5. For the luminosities probed here (~L*), we find that star formation rates (SFRs) and stellar masses of galaxies, with and without Lyα in emission, show small differences such that, LAEs have lower SFRs and stellar masses compared to non-LAEs. This result could be a direct consequence of the sample selection. Our sample of LAEs are selected based on their continuum magnitudes and they probe higher continuum luminosities compared to narrow-band/emission line selected LAEs. Based on our results, it is important to note that all LAEs are not universally similar and their properties are strongly dependent on the sample selection, and/or continuum luminosities.
Probabilistic Selection of High-redshift Quasars with Subaru/Hyper Suprime-Cam Survey
Authors: Onoue Masafusa 
Published: August 2016

AbstractHigh-redshift quasars are an important probe of the distant Universe. They enable observational studies of the early growth of supermassive blackholes, cosmic reionization, chemical enrichment of host galaxies, and so on. Through pioneering optical and near-infrared wide-area surveys such as the SDSS and the VIKING Survey, about one hundred quasars have been found at z > 6 (e.g., Fan et al. (2006b), Venemans et al. (2013)). However, its current small sample size and the fact that most of them are the most luminous (M1450 ≲ −24) population in this epoch prevents one from constraining statistics on high-redshift quasars, namely quasar luminosity function (QLF), and redshift evolution of IGM neutral fraction. Thus, discovery of large number of z > 6 quasars, especially low-luminous or z > 7 quasars, is highly desired for further understanding of the early universe.We are now starting a new ground-breaking survey of high-redshift (z > 6) quasars using the exquisite imaging data provided by the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) Survey. Thanks to its extremely wide coverage and its high sensitivity thorough five optical bands (1,400 deg2 to the depth of r ~ 26 in HSC-Wide layer), it is one of the most powerful contemporary surveys that makes it possible for us to increase the number of z > 6 quasars by almost an order of magnitude, i.e., 300 at z ~ 6 and 50 at z ~ 7, based on the current estimate of the QLF at z > 6 by Willott et al. (2010b).One of the biggest challenges in z > 6 quasar candidate selection is contamination of Galactic brown dwarfs, which have the same point-like appearance as and similarly red colors to the quasars. To overcome this issue and maximize the selection efficiency, we apply a double-layered approach to the HSC survey products, namely combination of two probabilistic selections: SED-fitting and Bayesian selection. In particular, we have developed a template SED fitting method optimized to high-redshift quasars selection. Its application with 27 photometric bands to the COSMOS quasars at 3 < z < 5 have shown that almost all of the known quasars are correctly classified with small dispersion σ|Δz|/(1+z)=0.01 and as low as η=2.5% outlier rate. At present, the HSC survey have successfully covered ~100 deg2 of HSC-Wide area in full colors. From the first-year data products, we have already started z > 6 quasar selection, and it is expected that the first HSC quasar discovery will be in the near future.
Galaxy morphologies in the era of big-data surveys
Authors: Huertas-Company M. 
Published: August 2016

AbstractGalaxy morphology is a first-order descriptor of a galaxy and a useful proxy to identify physical processes. The 100 years old Hubble fork describes the structural diversity of galaxies in the local universe. Unveiling the origins of this galaxy zoology is a key challenge in galaxy evolution. In this review talk, I first summarized some key advances in our understanding of the morphological evolution of galaxies from z ~ 0 to z ~ 3, thank you in particular to the SDSS and HST legacies. In the second part, I focused on the classification techniques. With the emergence in the last years of large surveys the samples of study have increased by several orders of magnitude going from a few tens to several millions of objects. This trend will clearly continue in the next decade with coming surveys/missions such as EUCLID and WFIRST. While galaxy classification is still a required step in any survey, visual inspection of galaxies is becoming prohibitively time-consuming. Under these circumstances, the techniques used to estimate galaxy morphologies need to be updated.
Minor mergers: fundamental but unexplored drivers of galaxy evolution
Authors: Kaviraj Sugata 
Published: August 2016

AbstractWe use the SDSS Stripe 82 to study the stellar-mass growth that is triggered by minor mergers in local disk galaxies. Since major mergers destroy disks and create spheroids, morphologically disturbed spirals are likely remnants of minor mergers (since the disk remains intact). Disturbed spirals exhibit enhanced specific star formation rates (SSFRs), with the enhancement increasing in galaxies with ‘later’ morphological type (that have larger gas reservoirs and smaller bulges). By combining the SSFR enhancements with the fraction of time spirals in various morphological classes spend in this ‘enhanced’ mode, we estimate that ~40% of the star formation activity in local spirals is directly triggered by minor mergers. Combining our results with the star formation in local early-type galaxies – which is almost completely driven by minor mergers – suggests that around half the star formation activity at the present day is likely to be triggered by the minor-merger process.
Public Choice barriers to efficient climate adaptation – theoretical insights and lessons learned from German flood disasters
Authors: GAWEL ERIK , LEHMANN PAUL , STRUNZ SEBASTIAN , HEUSON CLEMENS 
Published: August 2016

AbstractIn this paper, we take a Public Choice perspective to identify and categorise barriers to efficient public climate adaptation. Specifically, we distinguish three dimensions of public adaptation: extent, structure (form and timing) and organisation (coordination across territorial authorities and policy fields). Within each of these dimensions, we investigate how the self-interest of voters, pressure groups, bureaucrats and politicians may bias adaptation decisions. Thus, we indicate specific barriers to efficient public adaptation. Based on this framework, we illustrate how Germany's response to major flood disasters reflects the incentive structure of concerned stakeholders and their political interaction. The ad hoc character of some public adaptation measures implies a clear bias from the efficient benchmark. In conclusion, we argue that the propositions of Public Choice theory shed some light on how empirical public adaptation processes unfold.
Neural correlates of two different types of extinction learning in the amygdala central nucleus
Authors: Iordanova Mihaela D. , Deroche Mickael L. D. , Esber Guillem R. , Schoenbaum Geoffrey 
Published: August 2016

AbstractExtinction is a fundamental form of memory updating in which one learns to stop expecting an event that no longer occurs. This learning ensues when one experiences a change in environmental contingencies, that is, when an expected outcome fails to occur (simple extinction), or when a novel inflated expectation of a double outcome (overexpectation) is in conflict with the real outcome, and is a process that has been linked to amygdala function. Here, we show that in rats, the same neuronal population in the amygdala central nucleus updates reward expectancies and behaviour in both types of extinction, and neural changes in one paradigm are reflected in the other. This work may have implications for the management of addiction and anxiety disorders that require treatments based on the outcome omission, and disorders such as obesity that could use overexpectation, but not omission strategies.
PARP3 is a sensor of nicked nucleosomes and monoribosylates histone H2BGlu2
Authors: Grundy Gabrielle J. , Polo Luis M. , Zeng Zhihong , Rulten Stuart L. , Hoch Nicolas C. , Paomephan Pathompong , Xu Yingqi , Sweet Steve M. , Thorne Alan W. , Oliver Antony W. , Matthews Steve J. , Pearl Laurence H. , Caldecott Keith W. 
Published: August 2016

AbstractPARP3 is a member of the ADP-ribosyl transferase superfamily that we show accelerates the repair of chromosomal DNA single-strand breaks in avian DT40 cells. Two-dimensional nuclear magnetic resonance experiments reveal that PARP3 employs a conserved DNA-binding interface to detect and stably bind DNA breaks and to accumulate at sites of chromosome damage. PARP3 preferentially binds to and is activated by mononucleosomes containing nicked DNA and which target PARP3 trans-ribosylation activity to a single-histone substrate. Although nicks in naked DNA stimulate PARP3 autoribosylation, nicks in mononucleosomes promote the trans-ribosylation of histone H2B specifically at Glu2. These data identify PARP3 as a molecular sensor of nicked nucleosomes and demonstrate, for the first time, the ribosylation of chromatin at a site-specific DNA single-strand break.
Rapid α-oligomer formation mediated by the Aβ C terminus initiates an amyloid assembly pathway
Authors: Misra Pinaki , Kodali Ravindra , Chemuru Saketh , Kar Karunakar , Wetzel Ronald 
Published: August 2016

AbstractSince early oligomeric intermediates in amyloid assembly are often transient and difficult to distinguish, characterize and quantify, the mechanistic basis of the initiation of spontaneous amyloid growth is often opaque. We describe here an approach to the analysis of the Aβ aggregation mechanism that uses Aβ-polyglutamine hybrid peptides designed to retard amyloid maturation and an adjusted thioflavin intensity scale that reveals structural features of aggregation intermediates. The results support an aggregation initiation mechanism for Aβ-polyQ hybrids, and by extension for full-length Aβ peptides, in which a modular Aβ C-terminal segment mediates rapid, non-nucleated formation of α-helical oligomers. The resulting high local concentration of tethered amyloidogenic segments within these α-oligomers facilitates transition to a β-oligomer population that, via further remodelling and/or elongation steps, ultimately generates mature amyloid. Consistent with this mechanism, an engineered Aβ C-terminal fragment delays aggregation onset by Aβ-polyglutamine peptides and redirects assembly of Aβ42 fibrils.
Asymmetric counteranion-directed Lewis acid organocatalysis for the scalable cyanosilylation of aldehydes
Authors: Zhang Zhipeng , Bae Han Yong , Guin Joyram , Rabalakos Constantinos , van Gemmeren Manuel , Leutzsch Markus , Klussmann Martin , List Benjamin 
Published: August 2016

AbstractDue to the high versatility of chiral cyanohydrins, the catalytic asymmetric cyanation reaction of carbonyl compounds has attracted widespread interest. However, efficient protocols that function at a preparative scale with low catalyst loading are still rare. Here, asymmetric counteranion-directed Lewis acid organocatalysis proves to be remarkably successful in addressing this problem and enabled a molar-scale cyanosilylation in quantitative yield and with excellent enantioselectivity. Also, the catalyst loading could be lowered to a part-per-million level (50 ppm: 0.005 mol%). A readily accessible chiral disulfonimide was used, which in combination with trimethylsilyl cyanide, turned into the active silylium Lewis acid organocatalyst. The nature of a peculiar phenomenon referred to as a “dormant period”, which is mainly induced by water, was systematically investigated by means of in situ Fourier transform infrared analysis.
Core-shell nanoscale coordination polymers combine chemotherapy and photodynamic therapy to potentiate checkpoint blockade cancer immunotherapy
Authors: He Chunbai , Duan Xiaopin , Guo Nining , Chan Christina , Poon Christopher , Weichselbaum Ralph R. , Lin Wenbin 
Published: August 2016

AbstractAdvanced colorectal cancer is one of the deadliest cancers, with a 5-year survival rate of only 12% for patients with the metastatic disease. Checkpoint inhibitors, such as the antibodies inhibiting the PD-1/PD-L1 axis, are among the most promising immunotherapies for patients with advanced colon cancer, but their durable response rate remains low. We herein report the use of immunogenic nanoparticles to augment the antitumour efficacy of PD-L1 antibody-mediated cancer immunotherapy. Nanoscale coordination polymer (NCP) core-shell nanoparticles carry oxaliplatin in the core and the photosensitizer pyropheophorbide-lipid conjugate (pyrolipid) in the shell (NCP@pyrolipid) for effective chemotherapy and photodynamic therapy (PDT). Synergy between oxaliplatin and pyrolipid-induced PDT kills tumour cells and provokes an immune response, resulting in calreticulin exposure on the cell surface, antitumour vaccination and an abscopal effect. When combined with anti-PD-L1 therapy, NCP@pyrolipid mediates regression of both light-irradiated primary tumours and non-irradiated distant tumours by inducing a strong tumour-specific immune response.