Infrared to millimetre photometry of ultra-luminous ir galaxies: new evidence favouring a 3-stage dust model

By U. Klaas, M. Haas, S. Mueller, Rolf Chini, B. Schulz, I. Coulson, H. Hippelein, K. Wilke, M. Albrecht, D. Lemke. 2001

156 citations recorded by the source corpus.

Infrared to millimetre spectral energy distributions (SEDs) have been obtained for 41 bright ultra- luminous infrared galaxies (ULIRGs). The observations were carried out with ISOPHOT between 10 and 200 m and supplemented for 16 sources with JCMT/SCUBA at 450 and 850 m and with SEST at 1.3 mm. In addition, seven sources were observed at 1.2 and 2.2 m with the 2.2 m telescope on Calar Alto. These new SEDs represent the most complete set of infrared photometric templates obtained so far on ULIRGs in the local universe. The SEDs peak at 60{100 m and show often a quite shallow Rayleigh-Jeans tail. Fits with one single modied blackbody yield a high FIR opacity and small dust emissivity exponent T >30 K) to cold (30 K >T >10 K) temperatures. This provides evidence for two dust stages, the cool starburst dominated one and the cold cirrus-like one. The third stage with several hundred Kelvin warm dust is identied in the AGN dominated ULIRGs, showing up as a NIR-MIR power- law flux increase. While AGNs and SBs appear indistinguishable at FIR and submm wavelengths, they dier in the NIR-MIR. This suggests that the cool FIR emitting dust is not related to the AGN, and that the AGN only powers the warm and hot dust. In comparison with optical and MIR spectroscopy, a criterion based on the SED shapes and the NIR colours is established to reveal AGNs among ULIRGs. Also the possibility of recognising evolutionary trends among the ULIRGs via the relative amounts of cold, cool and warm dust components is investigated.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1bf03b67c45add1161bba75e9307f36eddb4281d

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Citations in the corpus

• Early Growth and Efficient Accretion of Massive Black Holes at High Redshift (2003, background): “This is (a) determined from CO emission line measurements (Ohta et al. 1996; Omont et al. 1996; Guilloteau et al. 1999; Carilli et al. 1999, 2002a, 2002b; Papadopoulos et al. 2000), and (b) inferred from the dust masses and typical dust-to-gas ratios obtained from low-z starbursts (e.g., Sanders, Sc”
• Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. IV. The Controlling Parameters of the Starburst SED (2007, methodology): “The majority of data points in the 1–1300µm wavelength range come from Klaas et al. (1997, 2001).”
• Spitzer Quasar and ULIRG Evolution Study (QUEST). II. The Spectral Energy Distributions of Palomar-Green Quasars (2007, result): “As for those sources with larger L(PAH) and L(FIR), the assumed ULIRG-like ratio is favored because of the similar luminosity to the QUEST ULIRGs.”
• SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS (2009, methodology): “The far-infrared photometry is mostly from the IRAS Faint Source Catalog, but also includes some data from Sanders et al. (2003) and a few ISO 12 µm points from Klaas et al. (2001).”
• Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. I. The Role of ISM Pressure and the Molecular Cloud Dissipation Timescale (2004, background): “M orecom plex m ulti-tem perature tsdo a betterjob in thisregard (see e.g.Klaas et al.2001),but allsuch tting is fundam entally unphysical.”
• Starburst and AGN activity in ultraluminous infrared galaxies (2003, methodology): “Other infrared data were taken from Carico et al (1988); Maiolino et al (1995); Klaas et al (1997); Rigopoulou et al (1999); Dale et al (2000); Zink et al (2000); Tran et al (2001) & Klaas et al (2001).”
• ON THE EFFECT OF THE COSMIC MICROWAVE BACKGROUND IN HIGH-REDSHIFT (SUB-)MILLIMETER OBSERVATIONS (2013, methodology): “…galaxy SEDs by comparing them with modified black body (MBB) functions (of the formνβ Bν [Tdust]) that describe the emission by dust in thermal equilibrium using only three parameters: the dust emissivity indexβ, temperatureTdust, and total luminosity (e.g. Dunne et al. 2000; Klaas et al. 2001).”
• Fitting the integrated spectral energy distributions of galaxies (2010, background): “This reflects a real dearth of specialized codes for carrying out the fitting process in the dust emission range (besides simple χ2 minimization over a parameter grid, e.g. Klaas et al. 2001).”
• The ISO view of Palomar-Green quasars (2003, methodology): “For comparison, the near- to mid-infrared SEDs of the four warm ULIRGs IRAS 05189-2524, Mrk 231, Mrk 463 and IRAS 19254-7245 (Klaas et al. 2001) can also be fitted by a power law with a mean α = −1.6 ± 0.05, which lies at the steep end of the slope distribution for the PG quasars.”
• A Compendium of Far-Infrared Line and Continuum Emission for 227 Galaxies Observed by the Infrared Space Observatory (2008, methodology): “Using published fluxes from ISOPHOT pointed observations at 180 µm (Klaas et al. 2001) and 170 µm Serendipity Survey (Stickel et al. 2000), 25 galaxies constrained to the LWS beam are compared to 170 µm fluxes measured by the LWS.”
• Infrared Power-Law Galaxies in the Chandra Deep Field-South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies (2006, background): “ULIRGs (LIR > 10 12 L ) containing an AGN, in particular warm ULIRGs, also have near- and mid-IR SEDs resembling power laws (see Sanders et al. 1988; Klaas et al. 2001).”
• Spitzer Quasar and ULIRG Evolution Study (QUEST). I. The Origin of the Far-Infrared Continuum of QSOs (2006, background): “Issues discussed in IRAS and ISO studies include the nature of ultraluminous infrared galaxies and their starburst andAGNenergy sources (Genzel et al. 1998;Klaas et al. 2001), and the spectral energy distributions (SEDs) of QSOs and their evolutionary implications (Haas et al. 2003).”
• Modelling infrared galaxy evolution using a phenomenological approach (2002, background): “(iii) Finally, we broaden the far-IR peak (also a continuous change with luminosity) and slightly flatten the long-wavelength spectrum (Dunne et al. 2000; Dunne & Eales 2001; Klaas et al. 2001).”
• Molecular line emission in NGC 1068 imaged with ALMA: I. An AGN-driven outflow in the dense molecular gas (2014, unknown): “…S ν, can be expressed as S ν = Mdust × κν × Bν(Tdust)/D2, where the emissivity of dust, κν, scales as ∼ κ352 GHz × (ν[GHz]/352)β, with κ352 GHz = 0.09 m2 kg−1 (a value rounded up from κ352 GHz = 0.0865 m2 kg−1 used by Klaas et al. 2001), Bν(Tdust) is the Planck function, and D is the distance.”
• Luminous Infrared Galaxies with the Submillimeter Array. I. Survey Overview and the Central Gas to Dust Ratio (2008, methodology): “Klaas et al. (2001) simply adopt an uncertainty of 30%.”
• The Herschel census of infrared SEDs through cosmic time (2013, background): “In order to calculate dust temperatures, we use a modified blackbody function (a grey-body), of the form Bλ(T )(1 − e−τλ ), with a wavelength-dependent optical depth τλ = τ100 μm(100 μm/λ)β (e.g. see Klaas et al. 2001) and a dust emissivity index β.”
• The Infrared Spectral Energy Distribution of Normal Star-forming Galaxies: Calibration at Far-Infrared and Submillimeter Wavelengths (2000, unknown): “See also Klaas et al. (2001) and Haas et al.”
• Dust in starburst nuclei and ULIRGs - SED models for observers (2006, unknown): “Typical mean values areTd = 10. . .20K (Krügel et al. 1998) and Tc = 30. . .50 K (Klaas et al. 2001).”