astro-ph
![arxiv: v2 [astro-ph] 1 Aug 2008](data:image/gif;base64,R0lGODlhAQABAIAAAP///wAAACH5BAEAAAAALAAAAAABAAEAAAICRAEAOw==)
arxiv: v2 [astro-ph] 1 Aug 2008
... In both cases, larger offsets resulting from large recoil kicks are more easily observable, but large kicks imply a small disk bound to the BH and thus a short off-center quasar duty cyc[r] ...
16
arxiv: v2 [astro-ph.he] 4 Nov 2013
... Besides the variability of the composite Fe K α line profiles, the properties of the observed SMBH bina- ries could be also constrained by studying the light curves of the different part[r] ...
8
arxiv: v2 [astro-ph.ga] 12 Dec 2014
... The blue solid line is the linear slope fit (#7 in Table 1) and the black dashed line the fit to the long period Cepheid sample (#8 in Table 1).... Same as Fig..[r] ...
72
arxiv: v1 [astro-ph.sr] 28 Dec 2017
... The last ones show complex P-Cygni features (clearly seen in the du Pont spectra and Nov 2015 FEROS spectra) with remarkable variations in the intensity of the absorption component.. Sod[r] ...
17
arxiv: v1 [astro-ph.ga] 20 May 2014
... The R12 F160W PLR is shown as a green solid line, the PLR for the long period Cepheids (#5 in Table 1) as a dashed black line and the the long period part of the broken slope PLR (#3 in [r] ...
49
arxiv: v2 [astro-ph.sr] 1 Dec 2017
... Comparison of cross-correlation function (CCF) profiles obtained from 3D synthetic spectra with velocities from the 3D simulation shows that the tomographic method correctly recovers the[r] ...
12
arxiv: v1 [astro-ph.sr] 10 Dec 2020
... (SPHERE) instrument at the Very Large Telescope (VLT), our goal is to acquire high contrast multi-epoch observations of three Sirius-like systems, HD 2133, HD 114174, and CD-56 7708 and [r] ...
19
arxiv: v1 [astro-ph.co] 20 Sep 2012
... Despite indirect photometric indications of the presence of a bar (e.g., star-forming ring, Type II sur- face brightness profile) and the faint (0.7% of the total light) detection in our[r] ...
15
arxiv: v1 [astro-ph.ga] 7 Mar 2016
... The presence of a break in the measured Lick indices and the clearly distinct distribution of the stellar population parameters for the inner galaxy ( R < R e) and the external halo p[r] ...
19
arxiv: v2 [astro-ph.ga] 22 Jul 2013
... The total number of YSOs within these clusters is between 4 000 and 8 000 stars depending on the cluster locations along the line of sight with respect to the parent molecular cloud.. Th[r] ...
11
arxiv: v1 [astro-ph.sr] 18 Apr 2009
... They also argued against a hybrid small-angle solution – one where the high-energy portion of the 8 B flux experiences an adiabatic crossing, suppressing these neutrinos, while the lowes[r] ...
23
arxiv: v1 [astro-ph.ep] 12 Feb 2014
... Using 3D hydrodynamical simulations including radiative transfer we have computed the torque acting on small mass planets kept on fixed or- bits in the aim of finding the critical mass f[r] ...
17
arxiv: v1 [astro-ph.he] 16 Aug 2009
... An unified picture of the afterglow light curve and prompt emission properties can be obtained with an o ff -axis geometry, suggesting that late and shallow rising optical light curves o[r] ...
10
arxiv: v2 [astro-ph.co] 25 Apr 2013
... However, analysis of blue galaxies in other HeCS clusters ( § 5. 3) shows no significant color dependence of the veloc- ity distribution of members identified with large redshift samples a[r] ...
31
arxiv: v1 [astro-ph.sr] 20 Mar 2018
... On the other hand, the less massive component is eclipsed during the primary (deeper) minimum of the light curves of W–type systems where the occultation of the more massive component ta[r] ...
17
arxiv: v1 [astro-ph.co] 15 Mar 2010
... Using the results from Section 3.3 we present the completeness and stellar corrected normalized di ff erential source counts per steradian ((dN / dS )S 2. 5 ) in the AKARI L15 15 µ m ban[r] ...
10
arxiv: v1 [astro-ph.co] 18 Sep 2014
... We are now in a position to observer how DCE experiments could be used to simulate (p)reheating in inflation methods via the modulation of time-dependent properties in quantum optics. On[r] ...
12
arxiv: v2 [astro-ph.he] 31 Oct 2014
... 6 shows a similar comparison be- tween the last observed spectrum of Dougie (+37 days after first light, or +30 days after the peak of the light curve, both measured in rest-frame) and s[r] ...
14
arxiv: v1 [astro-ph.ep] 20 Oct 2014
... In Figure 1 we plot the flux di ff erence between the transit light curve of an ellipsoidal and a spherical planet for some real close-in planets, chosen with di ff erent inclinations an[r] ...
6
arxiv: v1 [astro-ph.co] 31 May 2010
... We present the second report of our systematic search for strongly lensed quasars from the data of the Sloan Digital Sky Survey (SDSS). From extensive follow-up observations of 136 candi[r] ...
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