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12473133 | 1607.01526 | Globular clusters as tracers of the host galaxy mass distribution: the Fornax dSph test case | The Fornax dwarf spheroidal galaxy is the most massive satellites of the Milky Way, claimed to be embedded in a huge dark matter halo, and the only among the Milky Way satellites hosting five globular clusters. Interestingly, their estimated masses, ages and positions seem hardly compatible with the presence of a significant dark matter component, as expected in the ΛCDM scheme. Indeed, if Fornax would have a CDM halo with a standard density profile, all its globular clusters should have sunk to the galactic centre many Gyr ago due to dynamical friction. Due to this, some authors proposed that the most massive clusters may have formed out of Fornax and later tidally captured. In this paper, we investigate the past evolution of the Fornax GC system by using both a recently developed, semi-analytical treatment of dynamical friction and direct N-body simulations of the orbital evolution of the globular clusters within Fornax and of Fornax galaxy around the Milky Way. Our results suggest that an `in situ' origin for all the clusters is likely if their observed positions are close to their spatial ones and their orbits are almost circular. Moreover, the Milky Way seems to accelerate the GC decay reducing the decay time of 15 per cent. Nevertheless, our results indicate that the GCs survival probability exceeds 50 per cent, even in the case of cuspy density profiles. We conclude that more detailed data are required to shed light on the Fornax dark matter content, to distinguish between a cuspy or a cored profile. | [
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-0.... | 9.992026 | 7.407736 | 2016-07-01 | 17 | 2016MNRAS.461.4335A | [
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"five globular clusters",
"the globular clusters",
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... | [
"methods: numerical",
"galaxies: individual: Fornax",
"galaxies: nuclei",
"galaxies: star clusters: general",
"Astrophysics - Astrophysics of Galaxies"
] | 1 | [
"10.1093/mnras/stw1647",
"10.48550/arXiv.1607.01526"
] | [
"Arca-Sedda, M.",
"Capuzzo-Dolcetta, R."
] | [
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy",
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy"
] | [
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12410206 | 1607.02596 | Large-scale fluctuations in the number density of galaxies in independent surveys of deep fields | New arguments supporting the reality of large-scale fluctuations in the density of the visible matter in deep galaxy surveys are presented. A statistical analysis of the radial distributions of galaxies in the COSMOS and HDF-N deep fields is presented. Independent spectral and photometric surveys exist for each field, carried out in different wavelength ranges and using different observing methods. Catalogs of photometric redshifts in the optical (COSMOS-Zphot) and infrared (UltraVISTA) were used for the COSMOS field in the redshift interval 0.1 < z < 3.5, as well as the zCOSMOS (10kZ) spectroscopic survey and the XMM-COSMOS and ALHAMBRA-F4 photometric redshift surveys. The HDFN-Zphot and ALHAMBRA-F5 catalogs of photometric redshifts were used for the HDF-N field. The Pearson correlation coefficient for the fluctuations in the numbers of galaxies obtained for independent surveys of the same deep field reaches R = 0.70 ± 0.16. The presence of this positive correlation supports the reality of fluctuations in the density of visible matter with sizes of up to 1000 Mpc and amplitudes of up to 20% at redshifts z ~ 2. The absence of correlations between the fluctuations in different fields (the correlation coefficient between COSMOS and HDF-N is R = -0.20 ± 0.31) testifies to the independence of structures visible in different directions on the celestial sphere. This also indicates an absence of any influence from universal systematic errors (such as "spectral voids"), which could imitate the detection of correlated structures. | [
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0.... | 11.799792 | 3.5501 | 2016-07-01 | 8 | 2016ARep...60..563S | [
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... | [
"Astrophysics - Cosmology and Nongalactic Astrophysics",
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] | 3 | [
"10.1134/S1063772916040107",
"10.48550/arXiv.1607.02596"
] | [
"Shirokov, S. I.",
"Lovyagin, N. Yu.",
"Baryshev, Yu. V.",
"Gorokhov, V. L."
] | [
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University of Architecture and Civil Engineering, St. Petersburg, Russia"
] | [
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12406007 | 1607.07534 | K band SINFONI spectra of two z ~ 5 submillimeter galaxy systems: upper limits to the unobscured star formation from [O II] optical emission line searches | We present deep SINFONI K-band integral field spectra of two submillimeter galaxy systems (SMG): BR 1202-0725 and J1000+0234, at z = 4.69 and 4.55, respectively. Spectra extracted for each object in the two systems do not show any signature of the [O II]λλ3726, 29 Å emission-lines, placing upper flux limits of 3.9 and 2.5 × 10<SUP>-18</SUP>erg s<SUP>-1</SUP> cm<SUP>-2</SUP>for BR 1202-0725 and J1000+0234, respectively. Using the relation between the star formation rate (SFR) and the luminosity of the [O II] doublet, we estimate unobscured SFR upper limits of ~ 10-15 M<SUB>⊙</SUB> yr<SUP>-1</SUP>and ~30-40 M<SUB>⊙</SUB> yr<SUP>-1</SUP>for the objects of the two systems, respectively. For the SMGs, these values are at least two orders of magnitude lower than those derived from SED and IR luminosities. The differences on the SFR values would correspond to internal extinction of, at least, 3.4-4.9 and 2.1-3.6 mag in the visual for BR 1202-0725 and J1000+0234 SMGs, respectively. The upper limit for the [O II]-derived SFR in one of the LAEs (Lyα2) in the BR1202-0725 system is at least one order of magnitude lower than the previous SFR derived from infrared tracers, while both estimates are in good agreement for Lyα1. The lower limits to the internal extinction in these two Lyman-alpha emitters are 0.6 mag and 1.3 mag, respectively. No evidence for [O II] emission associated with Lyα1 is identified in our data, implying that residuals of the K-band sky emission lines after subtraction in medium-band imaging data could provide the adequate flux. | [
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"galaxies: starburst",
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] | 3 | [
"10.1051/0004-6361/201628952",
"10.48550/arXiv.1607.07534"
] | [
"Couto, Guilherme S.",
"Colina, Luis",
"López, Javier Piqueras",
"Storchi-Bergmann, Thaisa",
"Arribas, Santiago"
] | [
"Universidade Federal do Rio Grande do Sul, IF, CP 15051, 91501-970, Porto Alegre, RS, Brazil ; Centro de Astrobiología (INTA-CSIC), Ctra de Torrejón a Ajalvir, km 4, 28850 Torrejón de Ardoz, Madrid, Spain",
"Centro de Astrobiología (INTA-CSIC), Ctra de Torrejón a Ajalvir, km 4, 28850 Torrejón de Ardoz, Madrid, S... | [
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12594280 | 1607.08005 | Similarities and uniqueness of Ly α emitters among star-forming galaxies at z = 2.5 | We conducted a deep narrow-band imaging survey with the Subaru Prime Focus Camera on the Subaru Telescope and constructed a sample of Lyα emitters (LAEs) at z = 2.53 in the UDS-CANDELS field, where a sample of Hα emitters (HAEs) at the same redshift is already obtained from our previous narrow-band observation at near-infrared. The deep narrow-band and multibroad-band data allow us to find LAEs of stellar masses and star formation rates (SFRs) down to ≳10<SUP>8</SUP> M<SUB>⊙</SUB> and ≳0.2 M<SUB>⊙</SUB> yr<SUP>-1</SUP>, respectively. We show that the LAEs are located along the same mass-SFR sequence traced by normal star-forming galaxies such as HAEs, but towards a significantly lower mass regime. Likewise, LAEs seem to share the same mass-size relation with typical star-forming galaxies, except for the massive LAEs that tend to show significantly compact sizes. We identify a vigorous mass growth in the central part of LAEs: the stellar mass density in the central region of LAEs increases as their total galaxy mass grows. On the other hand, we see no Lyα line in emission for most of the HAEs. Rather, we find that the Lyα feature is either absent or in absorption (Lyα absorbers, LAAs), and its absorption strength may increase with reddening of the UV continuum slope. We demonstrate that a deep Lyα narrow-band imaging like this study is able to search for not only LAEs but also LAAs in a certain redshift slice. This work suggests that LAEs trace normal star-forming galaxies in the low-mass regime, while they remain as a unique population because the majority of HAEs are not LAEs. | [
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-0... | 13.462973 | 6.428069 | 2016-07-01 | 17 | 2017MNRAS.468.1123S | [
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"a certain redshift slice",... | [
"galaxies: evolution",
"galaxies: formation",
"galaxies: high-redshift",
"Astrophysics - Astrophysics of Galaxies"
] | 12 | [
"10.1093/mnras/stx091",
"10.48550/arXiv.1607.08005"
] | [
"Shimakawa, Rhythm",
"Kodama, Tadayuki",
"Shibuya, Takatoshi",
"Kashikawa, Nobunari",
"Tanaka, Ichi",
"Matsuda, Yuichi",
"Tadaki, Ken-ichi",
"Koyama, Yusei",
"Hayashi, Masao",
"Suzuki, Tomoko L.",
"Yamamoto, Moegi"
] | [
"Department of Astronomical Science, SOKENDAI, Osawa, Mitaka, Tokyo 181-8588, Japan; National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan",
"Department of Astronomical Science, SOKENDAI, Osawa, Mitaka, Tokyo 181-8588, Japan; National Astronomical Observatory of Japan, Osawa, Mitaka, To... | [
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12472610 | 1607.02477 | Is there substructure around M87? | We present a general method to identify infalling substructure in discrete data sets with position and line-of-sight velocity data. We exploit the fact that galaxies falling on to a brightest cluster galaxy (BCG) in a virialized cluster, or dwarf satellites falling on to a central galaxy like the Milky Way, follow nearly radial orbits. If the orbits are exactly radial, we show how to find the probability distribution for a satellite's energy, given a tracer density for the satellite population, by solving an Abel integral equation. This is an extension of Eddington's classical formula for the isotropic distribution function. When applied to a system of galaxies, clustering in energy space can then be quantified using the Kullback-Leibler divergence, and groups of objects can be identified which, though separated in the sky, may be falling in on the same orbit. This method is tested using mock data and applied to the satellite galaxy population around M87, the BCG in Virgo, and a number of associations that are found, which may represent infalling galaxy groups. | [
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-0.... | 10.674732 | 6.126083 | 2016-07-01 | 7 | 2016MNRAS.462..298O | [
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"galaxies: individual: M87",
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] | 3 | [
"10.1093/mnras/stw1574",
"10.48550/arXiv.1607.02477"
] | [
"Oldham, L. J.",
"Evans, N. W."
] | [
"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK",
"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK"
] | [
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1486962 | 1607.07723 | Probing the physics and history of cosmic reionization with the Sunyaev-Zel'dovich effect | "Context. The evolution of the Universe during the dark ages (DA) and the epoch of reonization (EoR)(...TRUNCATED) | [0.04228117689490318,0.02670390158891678,-0.003186115762218833,0.00906116608530283,-0.01085805241018(...TRUNCATED) | 13.296888 | 3.253237 | 2016-07-01 | 5 | 2016A&A...595A..21C | ["SZE-21 cm","galaxy clusters","cosmic structures","radio galaxies","the non-thermal SZE-21 cm","gal(...TRUNCATED) | ["dark ages","reionization","first stars","galaxies: clusters: general","cosmic background radiation(...TRUNCATED) | 3 | [
"10.1051/0004-6361/201424904",
"10.48550/arXiv.1607.07723"
] | [
"Colafrancesco, S.",
"Marchegiani, P.",
"Emritte, M. S."
] | ["INAF-Osservatorio Astronomico di Roma via Frascati 33, 00040, Monteporzio, Italy ; School of Physi(...TRUNCATED) | ["2018arXiv181010115M","2019arXiv190312631M","2020Ap&SS.365..188T","2020PhRvD.101l3510N","2021MNRAS.(...TRUNCATED) | ["1952AJ.....57R..31W","1959ApJ...129..536F","1976A&A....49..137C","1990MNRAS.247..510S","1999PhR...(...TRUNCATED) |
11492527 | 1607.05383 | The Clustering of Luminous Red Galaxies at z ∼ 0.7 from EBOSS and BOSS Data | "We present the first scientific results from the luminous red galaxy (LRG) sample of the extended B(...TRUNCATED) | [0.06529414653778076,0.00021087960340082645,0.04679490998387337,0.011064634658396244,0.0118150757625(...TRUNCATED) | 12.117682 | 2.783309 | 2016-07-01 | 57 | 2017ApJ...848...76Z | ["massive galaxies","Baryon Oscillation Spectroscopic Survey","BOSS LOWZ","BOSS CMASS","fixed halo m(...TRUNCATED) | ["cosmology: observations","galaxies: evolution","large-scale structure of universe","Astrophysics -(...TRUNCATED) | 6 | [
"10.3847/1538-4357/aa8eee",
"10.48550/arXiv.1607.05383"
] | ["Zhai, Zhongxu","Tinker, Jeremy L.","Hahn, ChangHoon","Seo, Hee-Jong","Blanton, Michael R.","Tojeir(...TRUNCATED) | ["Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washingto(...TRUNCATED) | ["2017ApJ...839..121T","2017ApJS..233...25A","2017MNRAS.467.3533T","2017MNRAS.468...77E","2018ARA&A.(...TRUNCATED) | ["1980lssu.book.....P","1983ApJ...267..465D","1993ApJ...412...64L","1994MNRAS.266...50F","1996AJ....(...TRUNCATED) |
2526299 | 1607.03100 | Size matters: abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE | "The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, M<SUB>str</SUB>, to its ro(...TRUNCATED) | [0.020051706582307816,0.004345771856606007,0.059796832501888275,-0.012249702587723732,0.010266770608(...TRUNCATED) | 11.191223 | 6.156008 | 2016-07-01 | 45 | 2017MNRAS.464.4736F | ["galaxy assembly","galaxies","EAGLE galaxies","galaxy formation efficiency","stellar mass","disc si(...TRUNCATED) | ["Galaxy: formation","Galaxy: kinematics and dynamics","Galaxy: structure","Astrophysics - Astrophys(...TRUNCATED) | 16 | [
"10.1093/mnras/stw2691",
"10.48550/arXiv.1607.03100"
] | ["Ferrero, Ismael","Navarro, Julio F.","Abadi, Mario G.","Sales, Laura V.","Bower, Richard G.","Crai(...TRUNCATED) | ["Instituto de Astronomía Teórica y Experimental, CONICET-UNC, Laprida 854, X5000BGR, Córdoba, Ar(...TRUNCATED) | ["2017MNRAS.467.1965H","2017MNRAS.468.2283C","2017MNRAS.469.1054A","2017MNRAS.471.1841N","2017MNRAS.(...TRUNCATED) | ["1977A&A....54..661T","1979ApJ...229....1A","1984MNRAS.211..753B","1985ApJ...292..371D","1986ApJ...(...TRUNCATED) |
12472778 | 1607.05795 | "The anatomy of a star-forming galaxy: pressure-driven regulation of star formation in simulated gal(...TRUNCATED) | "We explore the regulation of star formation in star-forming galaxies through a suite of high-resolu(...TRUNCATED) | [-0.0036397792864590883,0.04058526083827019,-0.004738285206258297,0.004347079433500767,-0.0187653619(...TRUNCATED) | 11.714225 | 8.613326 | 2016-07-01 | 38 | 2016MNRAS.462.3053B | ["feedback sub-grid models","star formation","star formation parameters","simulated star formation r(...TRUNCATED) | ["methods: numerical","ISM: clouds","ISM: evolution","galaxies: evolution","galaxies: ISM","galaxies(...TRUNCATED) | 5 | [
"10.1093/mnras/stw1741",
"10.48550/arXiv.1607.05795"
] | [
"Benincasa, S. M.",
"Wadsley, J.",
"Couchman, H. M. P.",
"Keller, B. W."
] | ["Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada","Departmen(...TRUNCATED) | ["2017ApJ...845..133S","2017MNRAS.468.4189P","2018ApJ...861....4S","2018MNRAS.477.1903S","2018MNRAS.(...TRUNCATED) | ["1994ApJ...435L.121E","1998ApJ...498..541K","2003ApJ...587..278W","2003PASP..115..763C","2004ApJ...(...TRUNCATED) |
12408911 | 1607.03982 | Galaxy Groups in the 2Mass Redshift Survey | "A galaxy group catalog is constructed from the 2MASS Redshift Survey (2MRS) with the use of a halo-(...TRUNCATED) | [0.01128902193158865,0.004166906233876944,0.055985815823078156,0.0037861736491322517,-0.010394603013(...TRUNCATED) | 12.206766 | 5.244895 | 2016-07-01 | 26 | 2016ApJ...832...39L | ["other member galaxies","other group catalogs","galaxies","A galaxy group catalog","this group cata(...TRUNCATED) | ["dark matter","galaxies: halos","large-scale structure of universe","methods: statistical","Astroph(...TRUNCATED) | 10 | [
"10.3847/0004-637X/832/1/39",
"10.48550/arXiv.1607.03982"
] | ["Lu, Yi","Yang, Xiaohu","Shi, Feng","Mo, H. J.","Tweed, Dylan","Wang, Huiyuan","Zhang, Youcai","Li,(...TRUNCATED) | ["Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Nandan R(...TRUNCATED) | ["2017MNRAS.470.2982L","2018A&A...618A..81T","2018ApJ...858..110P","2018MNRAS.473.4318A","2018PhRvD.(...TRUNCATED) | ["1968ApJ...151..393S","1976ApJ...203..297S","1976ApJ...207..700F","1982ApJ...257..423H","1985ApJ...(...TRUNCATED) |
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