http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
Radio Selection of the Most Distant Galaxy Clusters
Daddi, E.,Jin, S.,Strazzullo, V.,Sargent, M. T.,Wang, T.,Ferrari, C.,Schinnerer, E.,Smolč,ić,, V.,Calabró,, A.,Coogan, R.,Delhaize, J.,Delvecchio, I.,Elbaz, D.,Gobat, R.,Gu, Q.,Liu, D. American Astronomical Society 2017 ASTROPHYSICAL JOURNAL LETTERS - Vol.846 No.2
Daddi, Vanita Rohit,Pawar, Yashashree Shivajirao Department of Mathematics 2012 Kyungpook mathematical journal Vol.52 No.4
We introduce the concepts of ordered quasi-ideals, ordered bi-ideals in an ordered ternary semigroup and study their properties. Also regular ordered ternary semigroup is defined and several ideal-theoretical characterizations of the regular ordered ternary semigroups are furnished.
An extremely young massive clump forming by gravitational collapse in a primordial galaxy
Zanella, A.,Daddi, E.,Le Floc’h, E.,Bournaud, F.,Gobat, R.,Valentino, F.,Strazzullo, V.,Cibinel, A.,Onodera, M.,Perret, V.,Renaud, F.,Vignali, C. Nature Publishing Group, a division of Macmillan P 2015 Nature Vol.521 No.7550
When cosmic star formation history reaches a peak (at about redshift z ≈ 2), galaxies vigorously fed by cosmic reservoirs are dominated by gas and contain massive star-forming clumps, which are thought to form by violent gravitational instabilities in highly turbulent gas-rich disks. However, a clump formation event has not yet been observed, and it is debated whether clumps can survive energetic feedback from young stars, and afterwards migrate inwards to form galaxy bulges. Here we report the spatially resolved spectroscopy of a bright off-nuclear emission line region in a galaxy at z = 1.987. Although this region dominates star formation in the galaxy disk, its stellar continuum remains undetected in deep imaging, revealing an extremely young (less than ten million years old) massive clump, forming through the gravitational collapse of more than one billion solar masses of gas. Gas consumption in this young clump is more than tenfold faster than in the host galaxy, displaying high star-formation efficiency during this phase, in agreement with our hydrodynamic simulations. The frequency of older clumps with similar masses, coupled with our initial estimate of their formation rate (about 2.5 per billion years), supports long lifetimes (about 500 million years), favouring models in which clumps survive feedback and grow the bulges of present-day galaxies.
Satellite content and quenching of star formation in galaxy groups at<i>z</i>~ 1.8
Gobat, R.,Daddi, E.,Bé,thermin, M.,Pannella, M.,Finoguenov, A.,Gozaliasl, G.,Le Floc’h, E.,Schreiber, C.,Strazzullo, V.,Sargent, M.,Wang, T.,Hwang, H. S.,Valentino, F.,Cappelluti, N.,Li, Y.,Hasi EDP Sciences 2015 Astronomy and astrophysics Vol.581 No.-
METAL DEFICIENCY IN CLUSTER STAR-FORMING GALAXIES AT<i>Z</i>= 2
Valentino, F.,Daddi, E.,Strazzullo, V.,Gobat, R.,Onodera, M.,Bournaud, F.,Juneau, S.,Renzini, A.,Arimoto, N.,Carollo, M.,Zanella, A. IOP Publishing 2015 The Astrophysical journal Vol.801 No.2
<P>We investigate the environmental effect on the metal enrichment of star-forming galaxies (SFGs) in the farthest spectroscopically confirmed and X-ray-detected cluster, CL J1449+0856 at z = 1.99. We combined Hubble Space Telescope/WFC3 G141 slitless spectroscopic data, our thirteen-band photometry, and a recent Subaru/Multi-object InfraRed Camera and Spectrograph (MOIRCS) near-infrared spectroscopic follow-up to constrain the physical properties of SFGs in CL J1449+0856 and in a mass-matched field sample. After a conservative removal of active galactic nuclei, stacking individual MOIRCS spectra of 6 (31) sources in the cluster (field) in the mass range 10 <= log(M/M-circle dot) <= 11, we find a similar to 4 sigma. lower [N II]/H alpha ratio in the cluster than in the field. Stacking a subsample of 16 field galaxies with H beta and [O III] in the observed range, we measure an [O III]/H beta ratio fully compatible with the cluster value. Converting these ratios into metallicities, we find that the cluster SFGs are up to 0.25 dex poorer in metals than their field counterparts, depending on the adopted calibration. The low metallicity in cluster sources is confirmed using alternative indicators. Furthermore, we observe a significantly higher H alpha luminosity and equivalent width in the average cluster spectrum than in the field. This is likely due to the enhanced specific star formation rate; even if lower dust reddening and/or an uncertain environmental dependence on. the continuum-to-nebular emission differential reddening may play a role. Our findings might be explained by the accretion of pristine gas around galaxies at z = 2 and from cluster-scale reservoirs, possibly connected with a phase of rapid halo mass assembly at z > 2 and of a high galaxy merging rate.</P>
The [C ii] emission as a molecular gas mass tracer in galaxies at low and high redshifts
Zanella, A,Daddi, E,Magdis, G,Diaz Santos, T,Cormier, D,Liu, D,Cibinel, A,Gobat, R,Dickinson, M,Sargent, M,Popping, G,Madden, S C,Bethermin, M,Hughes, T M,Valentino, F,Rujopakarn, W,Pannella, M,Bourna Oxford University Press 2018 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.481 No.2