Results 51 to 60 of about 73,764 (311)

The Dragonfly Galaxy. III. Jet Brightening of a High-redshift Radio Source Caught in a Violent Merger of Disk Galaxies

open access: yesThe Astrophysical Journal, 2023
The Dragonfly galaxy (MRC 0152-209), the most infrared-luminous radio galaxy at redshift z ∼ 2, is a merger system containing a powerful radio source and large displacements of gas.
Sophie Lebowitz   +10 more
doaj   +1 more source

SGAS 143845.1+145407: A Big, Cool Starburst at Redshift 0.816 [PDF]

open access: yes, 2012
We present the discovery and a detailed multi-wavelength study of a strongly-lensed luminous infrared galaxy at z=0.816. Unlike most known lensed galaxies discovered at optical or near-infrared wavelengths this lensed source is red, r-Ks = 3.9 [AB ...
Abramson, Louis E.   +16 more
core   +3 more sources

Spectroscopy of Luminous Infrared Galaxies [PDF]

open access: yesSymposium - International Astronomical Union, 1999
A review of recent optical and infrared spectroscopic results on luminous infrared galaxies is presented. The main emphasis is on the ultraluminous objects. Possible correlations with infrared luminosity are identified. These results are used to constrain the nature of the dominant energy source in luminous infrared galaxies, and to test whether these ...
openaire   +1 more source

Spatially resolved kinematics, galactic wind, and quenching of star formation in the luminous infrared galaxy IRAS F11506-3851 [PDF]

open access: yes, 2014
We present a multi-wavelength integral field spectroscopic (IFS) study of the low-z luminous infrared galaxy IRAS F11506-3851 (ESO 320-G030) on the basis of the moderate spectral resolution observations (R 3400 4000) taken with the VIMOS and SINFONI ...
S. Cazzoli   +6 more
semanticscholar   +1 more source

A Large Mass of H2 in the Brightest Cluster Galaxy in Zwicky 3146 [PDF]

open access: yes, 2006
We present the Spitzer/IRS mid-infrared spectrum of the infrared-luminous (L_{IR}=4e11 L_sun) brightest cluster galaxy (BCG) in the X-ray-luminous cluster Z3146 (z=0.29).
Allen S. W.   +7 more
core   +2 more sources

DISCOVERY OF GeV EMISSION FROM THE DIRECTION OF THE LUMINOUS INFRARED GALAXY NGC 2146 [PDF]

open access: yes, 2014
Recent detections of high-energy gamma-ray emission from starburst galaxies M82 and NGC 253 suggest that starburst galaxies are huge reservoirs of cosmic rays and these cosmic rays convert a significant fraction of their energy into gamma-rays by ...
Q. Tang   +2 more
semanticscholar   +1 more source

Evolution of the ISM in luminous infrared galaxies [PDF]

open access: yesAstronomy and Astrophysics, 2010
Aims. Molecules that trace the high-density regions of the interstellar medium may be used to evaluate the changing physical and chemical environment during the ongoing nuclear activity in (ultra-) luminous infrared galaxies (ULIRGs).Methods. The changing ratios of the HCN (1-0), HNC (1-0), HCO(+) (1-0), CN (1-0) and CN (2-1), and CS (3-2) transitions ...
Baan, W. A., Loenen, A. F., Spaans, M.
openaire   +2 more sources

A MULTI-WAVELENGTH VIEW OF THE CENTRAL KILOPARSEC REGION IN THE LUMINOUS INFRARED GALAXY NGC 1614 [PDF]

open access: yes, 2014
The Luminous Infrared Galaxy NGC 1614 hosts a prominent circumnuclear ring of star formation. However, the nature of the dominant emitting mechanism in its central ∼100 pc is still under debate.
R. Herrero-Illana   +11 more
semanticscholar   +1 more source

Fading AGNs in Poststarburst Galaxies

open access: yesThe Astrophysical Journal, 2023
The role of active galactic nuclei (AGNs) in quenching galaxies and driving the evolution from star forming to quiescence remains a key question in galaxy evolution.
K. Decker French   +6 more
doaj   +1 more source

A Diverse Population of z ∼ 2 ULIRGs Revealed by JWST Imaging

open access: yesThe Astrophysical Journal, 2023
Four ultraluminous infrared galaxies (ULIRGs) observed with JWST/NIRcam in the Cosmos Evolution Early Release Science program offer an unbiased preview of the z ∼ 2 ULIRG population.
J.-S. Huang   +14 more
doaj   +1 more source

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