Results 51 to 60 of about 35,402 (267)

The Most Luminous Galaxies [PDF]

open access: yes, 2002
Ultraluminous galaxies in the local universe (z$\leq$0.2) emit the bulk of their energy in the mid and far-infrared. The multiwavelength approach to these objects has shown that they are advanced mergers of gas-rich spiral galaxies.
Mirabel, I. Felix
core   +3 more sources

Resolved CO(1–0) Emission and Gas Properties in Luminous Dusty Star-forming Galaxies at z = 2–4

open access: yesThe Astrophysical Journal, 2023
We present the results of a survey of CO(1−0) emission in 14 infrared luminous dusty star-forming galaxies (DSFGs) at 2 < z < 4 with the NSF’s Karl G. Jansky Very Large Array.
F. Stanley   +17 more
doaj   +1 more source

Optical Properties of 4248 IRAS Galaxies

open access: yes, 2005
We have investigated optical properties of 4248 infrared galaxies (IRGs) by positionally matching data from the IRAS and the SDSS DR3. Our sample includes 3 hyper luminous infrared galaxies (L >10^13Lsun) and 178 ultra luminous infrared galaxies (10 ...
Abazajian   +84 more
core   +1 more source

Asca Observations of Luminous Infrared Starburst Galaxies [PDF]

open access: yesSymposium - International Astronomical Union, 1999
We present recent results of X-ray observations of two luminous infrared galaxies, NGC3690+IC694 (Arp299) and NGC1614 obtained by the Japanese X-ray astronomical satellite ASCA. Both galaxies have quite high infrared luminosity (> 1011L⊙) and strong evidence of merger.
T. Nakagawa   +3 more
openaire   +2 more sources

A relation of the PAH 3.3 um feature with star-forming activity for galaxies with a wide range of infrared luminosity

open access: yes, 2013
For star-forming galaxies, we investigate a global relation between polycyclic aromatic hydrocarbon (PAH) emission luminosity at 3.3 um, L_PAH3.3, and infrared (8-1000 um) luminosity, L_IR, to understand how the PAH 3.3 um feature relates to the star ...
Im, Myungshin   +6 more
core   +1 more source

The stellar, molecular gas and dust content of the host galaxies of two z~2.8 dust obscured quasars [PDF]

open access: yes, 2011
We present optical through radio observations of the host galaxies of two dust obscured, luminous quasars selected in the mid-infrared, at z=2.62 and z=2.99, including a search for CO emission.
Farrah, Duncan   +6 more
core   +3 more sources

ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data

open access: yesThe Astrophysical Journal, 2023
We present the results of our ALMA ≲0.5 kpc resolution dense molecular line (HCN and HCO ^+ J = 2–1, J = 3–2, and J = 4–3) observations of 12 nearby (ultra)luminous infrared galaxies ([U]LIRGs). After matching beam sizes of all molecular line data to the
Masatoshi Imanishi   +3 more
doaj   +1 more source

The Aromatic Features in Very Faint Dwarf Galaxies

open access: yes, 2009
We present optical and mid-infrared photometry of a statistically complete sample of 29 very faint dwarf galaxies (M_r > -15 mag) selected from the SDSS spectroscopic sample and observed in the mid-infrared with Spitzer IRAC. This sample contains nearby (
Abazajian   +53 more
core   +1 more source

Dense Molecular Gas Properties of the Central Kiloparsec of Nearby Ultraluminous Infrared Galaxies Constrained by ALMA Three Transition-line Observations

open access: yesThe Astrophysical Journal, 2023
We report the results of Atacama Large Millimeter/submillimeter Array (ALMA) 1–2 kpc resolution, three rotational transition-line ( J = 2–1, J = 3–2, and J = 4–3) observations of multiple dense molecular gas tracers (HCN, HCO ^+ , and HNC) for 10 nearby (
Masatoshi Imanishi   +3 more
doaj   +1 more source

ChAInGeS: The Chandra Arp Interacting Galaxies Survey

open access: yes, 2011
We have conducted a statistical analysis of the ultra-luminous X-ray point sources (ULXs; L(X) >= 10^39 erg/s) in a sample of galaxies selected from the Arp Atlas of Peculiar Galaxies.
Abazajian   +74 more
core   +1 more source

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