scholarly journals The Nature of the Emission-line Nebulae in Powerful Far-infrared Galaxies

1990 ◽  
Vol 124 ◽  
pp. 409-413
Author(s):  
Lee Armus ◽  
Timothy M. Heckman ◽  
George K. Miley
Keyword(s):  
Emission Line ◽  
Narrow Band ◽  
Broad Band ◽  
Far Infrared ◽  
Interacting Galaxies ◽  
Spectral Energy ◽  
Infrared Galaxies ◽  
Energy Distributions ◽  
Infrared Spectral ◽  
The Mean

AbstractWe discuss our program of narrow-band (Hα + [Nil]) imaging of a sample of 30 powerful far-infrared galaxies (FIRG’s) chosen to have far-infrared spectral energy distributions similar to the prototype FIRG’s Arp 220, NGC 3690, NGC 6240, and M82. The emission-line nebulae of these IR color-selected sample (ICSS) galaxies as a class are both impressively large (mean half light radius, r ~1.3 Kpc, and mean diameter, D ~16 Kpc) and luminous (LTOT ~108 Lo; uncorrected for internal extinction). The mean total Hα + [Nil] luminosity of the FIRG’s is comparable to that found for pairs of optically selected interacting galaxies (Bushouse, Lamb, and Werner 1988), but is a factor of ~5 greater than that of isolated spirals (Kennicutt and Kent 1983). Only ~25% of the nearby (z ≤ 0.10) FIRG’s have morphologies suggesting that large HII~regions contribuí significantly to their emission-line appearance. The broad-band morphologies of our IR color-selected galaxies fall into three major categories. Nearly 75% are single galaxy systems, with the remaining FIRG’s being either multiple nuclei systems, or members of interacting pairs. Since we see few (10%) currently interacting FIRG’s, yet many (80%) with highly distorted continuum morphologies, our IR color criteria may be preferentially selecting galaxies that have undergone highly inelastic, rapidly merging interactions.

scholarly journals Longslit Optical Spectroscopy of Powerful Far-Infrared Galaxies

1989 ◽  
Vol 134 ◽  
pp. 414-415
Author(s):  
Lee Armus ◽  
Timothy M. Heckman ◽  
George K. Miley
Keyword(s):  
Direct Evidence ◽  
Thermal Emission ◽  
Large Range ◽  
Far Infrared ◽  
Spectral Energy ◽  
Infrared Galaxies ◽  
Energy Distributions ◽  
Hii Region ◽  
The Galaxy ◽  
Infrared Spectral

It has been known since the IRAS mission that there exist galaxies with far-infrared luminosities of 1011–1012Lo, and LFTR/LB = 10–100. Through extensive modelling and observations of HII-region/molecular cloud complexes in the Galaxy, this infrared radiation is believed to be thermal emission from heated dust grains (c.f. review by Stein and Soifer 1983). While starburst models are consistent with the data over a large range in wavelength, direct evidence for sizeable populations of young stars is scarce, and in many cases the presence of an active nucleus either cannot be ruled out, or is required on the basis of energy considerations. In order to better understand the energy source responsible for heating the dust, we have undertaken a spectroscopic survey of galaxies chosen to have far-infrared spectral energy distributions similar to the prototypical class members Arp 220, NGC 6240, NGC 3690, and Mrk 231. It was required that between 25μ and 60μ, α ≤ −1.5, and that between 60μ and 100μ, α ≥ −0.5, where Sv α vα.

scholarly journals Feedback‐driven Evolution of the Far‐Infrared Spectral Energy Distributions of Luminous and Ultraluminous Infrared Galaxies

2007 ◽  
Vol 658 (2) ◽  
pp. 840-850 ◽  
Author(s):  
Sukanya Chakrabarti ◽  
T. J. Cox ◽  
Lars Hernquist ◽  
Philip F. Hopkins ◽  
Brant Robertson ◽  
...  
Keyword(s):  
Far Infrared ◽  
Spectral Energy ◽  
Infrared Galaxies ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
Ultraluminous Infrared Galaxies ◽  
Infrared Spectral

scholarly journals The Far‐Infrared Spectral Energy Distributions of X‐Ray–selected Active Galaxies

2003 ◽  
Vol 590 (1) ◽  
pp. 128-148 ◽  
Author(s):  
Joanna K. Kuraszkiewicz ◽  
Belinda J. Wilkes ◽  
Eric ◽  
J. Hooper ◽  
Kim K. McLeod ◽  
...  
Keyword(s):  
Far Infrared ◽  
Active Galaxies ◽  
Spectral Energy ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
X Ray ◽  
Infrared Spectral

scholarly journals Identifications of Faint IRAS Sources

1996 ◽  
Vol 171 ◽  
pp. 402-402
Author(s):  
M.W. Kümmel ◽  
S.J. Wagner
Keyword(s):  
Broad Band ◽  
Far Infrared ◽  
Power Laws ◽  
Point Sources ◽  
Spectral Energy ◽  
Energy Distributions ◽  
The North ◽  
Luminosity Functions ◽  
Error Circle ◽  
Radio Band

From overlapping scans in the IRAS all-sky survey and additional pointed observations the deepest far infrared survey before ISO exists in the region around the North Ecliptic Pole (NEP) (Hacking P. and Houck J.R., ApJS 63 p. 311). This survey contains detections up to 10 and fluxes up to 100 times fainter than the IRAS survey. In the central square degree around the NEP we combine the far IR-survey with deep radio data at 151 MHz and 1.5 GHz (Visser, A.E. et al., A&AS 110 p. 419, Kollgaard, R.I. et al., ApJS 93 p. 145) and own observation at 2.2μm (K′) and 435nm (B). The error circle around the IRAS source was chosen to include the true source with 85% probability (1.4 sigma). For 29 of the 32 IRAS sources we found at least one possible counterpart. Ten of the objects have multiple (up to four) counterparts in K′. Four of the IRAS sources have counterparts in the 1.5 GHz survey. The higher accuracy of the radio position (∼ 1″) allowed an unambiguous identification of the K′ counterpart. None of the IRAS sources could be found in the 151 MHz survey. The broad band spectra of the three galaxies with measured radio flux exhibit maximum emission between the radio band and 100μm which corresponds to emission by cool dust (< 50 K). Contrary to the infrared luminosity functions at 12μm and 60μm which show power laws, the K′ luminosity function is bimodal. The brightest K′ objects are all point sources. Due to the small number statistics the power law indices of the luminosity functions can not be distinguished. We find a linear relationship between the K′ flux and the flux at 60μm and 12μm over at least one decade. The large deviations by individual sources make an identification of the correct counterpart through this relation impossible. The spectral energy distributions of unambiguously identified sources span only one decade in energy (vSv), i.e. they have flat energy distributions. This suggests an identification of K′ objects with flat energy distribution in case of multiple counterparts.

scholarly journals WELL-SAMPLED FAR-INFRARED SPECTRAL ENERGY DISTRIBUTIONS OFz∼ 2 GALAXIES: EVIDENCE FOR SCALED UP COOL GALAXIES

2010 ◽  
Vol 725 (1) ◽  
pp. 742-749 ◽  
Author(s):  
Adam Muzzin ◽  
Pieter van Dokkum ◽  
Mariska Kriek ◽  
Ivo Labbé ◽  
Iara Cury ◽  
...  
Keyword(s):  
Far Infrared ◽  
Spectral Energy ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
Infrared Spectral

scholarly journals WHAT SHAPES THE FAR-INFRARED SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES?

2016 ◽  
Vol 818 (1) ◽  
pp. 62 ◽  
Author(s):  
Mohammadtaher Safarzadeh ◽  
Christopher C. Hayward ◽  
Henry C. Ferguson ◽  
Rachel S. Somerville
Keyword(s):  
Far Infrared ◽  
Spectral Energy ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
Infrared Spectral

scholarly journals J-PLUS: Synthetic galaxy catalogues with emission lines for photometric surveys

2019 ◽  
Vol 631 ◽  
pp. A82 ◽  
Author(s):  
David Izquierdo-Villalba ◽  
Raul E. Angulo ◽  
Alvaro Orsi ◽  
Guillaume Hurier ◽  
Gonzalo Vilella-Rojo ◽  
...  
Keyword(s):  
Emission Line ◽  
Narrow Band ◽  
Spectral Energy Distribution ◽  
Broad Band ◽  
Line Emission ◽  
Spectral Energy ◽  
Filter Method ◽  
Medium Band ◽  
Emission Line Galaxies ◽  
The Impact

We present a synthetic galaxy lightcone specially designed for narrow-band optical photometric surveys. To reduce time-discreteness effects, unlike previous works, we directly include the lightcone construction in the L-Galaxies semi-analytic model applied to the subhalo merger trees of the Millennium simulation. Additionally, we add a model for the nebular emission in star-forming regions, which is crucial for correctly predicting the narrow- and medium-band photometry of galaxies. Specifically, we consider, individually for each galaxy, the contribution of 9 different lines: Lyα (1216 Å), Hβ (4861 Å), Hα (6563 Å), [O II] (3727 Å, 3729 Å), [O III] (4959 Å, 5007 Å), [Ne III] (3870 Å), [O I] (6300 Å), [N II] (6548 Å, 6583 Å), and [S II] (6717 Å, 6731 Å). We validate our lightcone by comparing galaxy number counts, angular clustering, and Hα, Hβ, [O II], and [O III]5007 luminosity functions to a compilation of observations. As an application of our mock lightcones, we generated catalogues tailored for J-PLUS, a large optical galaxy survey featuring five broad-band and seven medium-band filters. We study the ability of the survey to correctly identify, with a simple three-filter method, a population of emission-line galaxies at various redshifts. We show that the 4000 Å break in the spectral energy distribution of galaxies can be misidentified as line emission. However, all significant excess (> 0.4 mag) can be correctly and unambiguously attributed to emission-line galaxies. Our catalogues are publicly released to facilitate their use in interpreting narrow-band surveys and in quantifying the impact of line emission in broad-band photometry.

scholarly journals Dust in FIR-bright ADF-S galaxies

2014 ◽  
Vol 10 (S309) ◽  
pp. 325-325
Author(s):  
K. Małek ◽  
A. Pollo ◽  
T. T. Takeuchi ◽  
V. Buat ◽  
D. Burgarella ◽  
...  
Keyword(s):  
Far Infrared ◽  
Spectral Energy ◽  
Infrared Galaxies ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
Star Forming ◽  
Luminous Infrared Galaxies

AbstractMultiwavelength Spectral Energy Distributions (SEDs) of far-infrared (FIR) galaxies detected in the AKARI South Ecliptic Poles Survey (ADF-S) allow to trace differences between [Ultra]-Luminous Infrared Galaxies ([U]LIRGS) and other types of star-forming galaxies (SF).

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