OBSERVATIONS OF Arp 220 USING<i>HERSCHEL</i>-SPIRE: AN UNPRECEDENTED VIEW OF THE MOLECULAR GAS IN AN EXTREME STAR FORMATION ENVIRONMENT

Rangwala, Naseem; Maloney, Philip R.; Glenn, J.; Wilson, C. D.; Rykala, Adam John; Isaak, K. G.; Baes, M.; Bendo, G. J.; Boselli, A.; Bradford, C. M.; Clements, D. L.; Cooray, Asantha; Fulton, T.; Imhof, P.; Kamenetzky, J.; Madden, S.; Mentuch, Erin; Sacchi, N.; Sauvage, M.; Schirm, M. R. P.; Smith, M.; Spinoglio, L.; Wolfire, M. G.

doi:10.1088/0004-637x/743/1/94

Cited by 266 publications

(494 citation statements)

References 95 publications

(89 reference statements)

Supporting

Mentioning

431

Contrasting

Order By: Relevance

“…A thorough investigation of the water emission in the HERUS sample is beyond the scope of the current work and will be reported on in a forthcoming paper; however, we note that our measured fluxes for the water lines in Mrk 231 and Arp 220 are consistent within the errors with the results of González-Alfonso et al (2010. Finally, in addition to the above species, we also detect HCO + /HOC + (6−5) at 537 GHz (557 μm) in IRAS 13120 −5453, and confirm the detection of both HCO + /HOC + and HCN at 532 GHz (562 μm) in Arp 220 Rangwala et al (2011). In Table 4 the water line fluxes as measured by the SPIRE FTS for the HERUS local ULIRGs are tabulated in units of 10 −18 Wm −2 .…”

Section: Fitted Spectrasupporting

confidence: 90%

“…The [N II] line is indicative of hot HII regions rather than the PDR and can be used to estimate the fraction of [C II] emission that comes from ionized gas, rather than from PDRs. In many cases, the [N II] line is partially resolved and relatively broad (see Figure 9) and a sinc-Gauss profile was used to model the line in many instances where FWHM of ∼300-400 km −1 were measured, Although broad, these widths are still significantly smaller than those in systems that unambiguously are shown to have massive outflows (e.g., Feruglio et al 2010;Cicone et al 2014) Water is the second most oxygenated molecule (following CO) in the warm interstellar medium of galaxies and has been detected by Herschel in observations of nearby ULIRGs (González-Alfonso et al 2010;Rangwala et al 2011;PereiraSantaella et al 2013). The HERUS ULIRGs are also found to be abundant in water lines, in particular the ortho-H 2 O lines, IRAS 23230-6926, IRAS 06206-6315), and where the water lines, although detected, are significantly weaker than the CO lines (IRAS 09022-3615, IRAS 10565+2448, NGC 6240).…”

Section: Fitted Spectramentioning

confidence: 99%

See 1 more Smart Citation

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

View full text Add to dashboard Cite

We present the Herschel SPIRE Fourier Transform Spectroscopy (FTS) atlas for a complete flux-limited sample of local ultraluminous infrared galaxies (ULIRGs) as part of the HERschel Ultra Luminous InfraRed Galaxy Survey (HERUS). The data reduction is described in detail and was optimized for faint FTS sources ,with particular care being taken for the subtraction of the background, which dominates the continuum shape of the spectra. To improve the final spectra, special treatment in the data reduction has been given to any observation suffering from artifacts in the data caused by anomalous instrumental effects. Complete spectra are shown covering 200-671 μm, with photometry in the SPIRE bands at 250, 350, and 500 μm. The spectra include near complete CO ladders for over half of our sample, as well as fine structure lines from [C I] 370 μm, [C I] 609 μm, and [N II] 205 μm. We also detect H 2 O lines in several objects. We construct CO spectral line energy distributions (SLEDs) for the sample, and compare their slopes with the far-infrared (FIR) colors and luminosities. We show that the CO SLEDs of ULIRGs can be broadly grouped into three classes based on their excitation. We find that the mid-J (5<J<8) lines are better correlated with the total FIR luminosity, suggesting that the warm gas component is closely linked to recent star formation. The higher J transitions do not linearly correlate with the FIR luminosity, consistent with them originating in hotter, denser gas that is unconnected to the current star formation. We conclude that in most cases more than one temperature component is required to model the CO SLEDs.

show abstract

Section: Fitted Spectrasupporting

confidence: 90%

Section: Fitted Spectramentioning

confidence: 99%

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

View full text Add to dashboard Cite

show abstract

“…The optical depth is τ(ν) is defined by τ(ν) = κ ν Σ dust and is commonly represented as τ(ν) = (ν/ν 0 ) β , where β is the spectral emissivity index and ν 0 is the frequency where optical depth equals unity (Draine, 2006), often assumed as = 3 THz from laboratory experiments (≈100µm) although the measured value from a number of galaxies tends more towards 1.5 THz (≈200µm Conley et al, 2011;Rangwala et al, 2011). The dust mass absorption coefficient has an identical frequency dependence, κ ν = κ 0 (ν/ν 0 ) β , since τ ≡ κΣ dust .…”

Section: Direct Modified Blackbody Sed Modelingmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

Self Cite

View full text Add to dashboard Cite

Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

show abstract

“…The , as well as a decrease with FIR color in star-forming galaxies (Malhotra et al 2001). Several hypotheses to explain the apparent line deficit in galaxies include (1) more dust screening at high ionization parameter (Luhman et al 2003;Abel et al 2009); (2) lower photoelectric efficiency due to charged small dust grains under intense radiation fields (Malhotra et al 2001;Croxall et al 2012); (3) lower photoelectric efficiency due to a decrease in the PAH abundance under hard radiation fields (Madden et al 2006;Rubin et al 2009); and (4) large dust optical depths leading to extinction of the emission lines (Papadopoulos et al 2010;Rangwala et al 2011). The dwarf galaxies extend the relative importance of the gas cooling to high values.…”

Section: Interpretation Of the [C Ii]/l Tir And [O I]/l Tir Trendsmentioning

confidence: 99%

TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

240

399

View full text Add to dashboard Cite

Context. The far-infrared (FIR) lines are important tracers of the cooling and physical conditions of the interstellar medium (ISM) and are rapidly becoming workhorse diagnostics for galaxies throughout the universe. There are clear indications of a different behavior of these lines at low metallicity that needs to be explored. Aims. Our goal is to explain the main differences and trends observed in the FIR line emission of dwarf galaxies compared to more metal-rich galaxies, and how this translates in ISM properties. ] 57 µm fine-structure cooling lines in a sample of 48 low-metallicity star-forming galaxies of the guaranteed time key program Dwarf Galaxy Survey. We correlate PACS line ratios and line-to-L TIR ratios with L TIR , L TIR /L B , metallicity, and FIR color, and interpret the observed trends in terms of ISM conditions and phase filling factors with Cloudy radiative transfer models. Results. We find that the FIR lines together account for up to 3 percent of L TIR and that star-forming regions dominate the overall emission in dwarf galaxies. Compared to metal-rich galaxies, the ratios of Harboring compact phases of a low filling factor and a large volume filling factor of diffuse gas, the ISM of low-metallicity dwarf galaxies has a more porous structure than that of metal-rich galaxies. Methods

show abstract

OBSERVATIONS OF Arp 220 USINGHERSCHEL-SPIRE: AN UNPRECEDENTED VIEW OF THE MOLECULAR GAS IN AN EXTREME STAR FORMATION ENVIRONMENT

Abstract: We present Herschel SPIRE-FTS observations of Arp 220, a nearby ultraluminous infrared galaxy. The FTS provides continuous spectral coverage from 1 The SPIRE beam shapes are not gaussian; the effective beam solid angle can be found in the Herschel Observer's manual.

Cited by 266 publications

References 95 publications

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Dusty star-forming galaxies at high redshift

TheHerschelDwarf Galaxy Survey

Contact Info

Product

Resources

About