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Andromeda IV, a solitary gas-rich dwarf galaxy
Rizzi, L.; Sharina, M. E.; Karachentsev, I. D. +4 more
Observations are presented of the isolated dwarf irregular galaxy And IV made with the Hubble Space Telescope Advanced Camera for Surveys and the Giant Metrewave Radio Telescope in the 21 cm H I line. We determine the galaxy distance of 7.17{±}0.31 Mpc using the Tip of Red Giant Branch method. The galaxy has a total blue absolute magnitude of -12.…
A global look at X-ray time lags in Seyfert galaxies
Kara, E.; Fabian, A.; Alston, W.
X-ray reverberation, where light-travel time delays map out the compact geometry around the inner accretion flow in supermassive black holes, has been discovered in several of the brightest, most variable and well-known bare Seyfert galaxies. In this work, we expand the study of X-ray time lags to all Seyfert galaxies in the XMM-Newton archive abo…
Spectroscopic Diagnostics of Solar Magnetic Flux Ropes Using Iron Forbidden Line
Cheng, X.; Ding, M. D.
In this Letter, we present Interface Region Imaging Spectrograph Fe xxi 1354.08 Å forbidden line emission of two magnetic flux ropes (MFRs) that caused two fast coronal mass ejections with velocities of ≥1000 km s-1 and strong flares (X1.6 and M6.5) on 2014 September 10 and 2015 June 22, respectively. The extreme-ultraviolet images at t…
Hot gas and magnetic arms of NGC 6946: Indications for reconnection heating?
Ehle, M.; Weżgowiec, M.; Beck, R.
Context. The grand-design face-on spiral galaxy
Aims:…
Probing the Dragonfish star-forming complex: the ionizing population of the young massive cluster Mercer 30
Herrero, A.; Urbaneja, M. A.; Najarro, F. +11 more
It has recently been claimed that the nebula, Dragonfish, is powered by a superluminous but elusive OB association. However, systematic searches in near-infrared photometric surveys have found many other cluster candidates in this region of the sky. Among these, the first confirmed young massive cluster was Mercer 30, where Wolf-Rayet stars were f…
New Constraints on the Molecular Gas in the Prototypical HyLIRGs BRI1202-0725 and BRI1335-0417
Momjian, E.; Walter, F.; Riechers, D. A. +6 more
We present Karl G Jansky Very Large Array observations of CO(J=2\to 1) line emission and rest-frame 250 GHz continuum emission of the Hyper-Luminous IR Galaxies (HyLIRGs) BRI 1202-0725 (z = 4.69) and BRI 1335-0417 (z = 4.41), with an angular resolution as high as 0.″15. Our low-order CO observations delineate the cool molecular gas, the fuel for s…
A new approach to the infrared photometric study of Be stars
Chen, P. S.; Liu, J. Y.; Shan, H. G.
In this paper, we have collected data for almost all Be stars known so far (1991 sources in total) and photometrically study their infrared properties. 2MASS, WISE, IRAS and Akari data are analysed. It is shown from several two-colour diagrams that from 1 to 60 µm, infrared excesses for the majority of Be stars are mainly due to the free-fre…
Photochemistry of forbidden oxygen lines in the inner coma of 67P/Churyumov-Gerasimenko
Gunell, H.; Altwegg, K.; Fuselier, S. A. +19 more
Observations of the green and red-doublet emission lines have previously been realized for several comets. We present here a chemistry-emission coupled model to study the production and loss mechanisms of the O(1S) and O(1D) states, which are responsible for the emission lines of interest for comet 67P/Churyumov-Gerasimenko. …
Major-Merger Galaxy Pairs at Z = 0: Dust Properties and Companion Morphology
Domingue, Donovan L.; Cao, Chen; Xu, C. Kevin +4 more
We present an analysis of dust properties of a sample of close major-merger galaxy pairs selected by K s magnitude and redshift. The pairs represent the two populations of spiral-spiral (S+S) and mixed morphology spiral-elliptical (S+E). The Code Investigating GALaxy Emission software is used to fit dust models to the Two Micron All S…
Interacting parametrized post-Friedmann method
Xu, Lixin; Richarte, Martín G.
We apply the interacting parametrized post-Friedmann (IPPF) method to coupled dark energy models where the interaction is proportional to dark matter density at background level. In the first case, the dark components are treated as fluids and the growth of dark matter perturbations only feel the interaction via the modification of background quan…