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Five of the eight galaxies are detected in both wavebands and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at lambda>40 micron. The FIR spectral energy distributions (SEDs) are best fitted by a combination of two modified Planck functions, with T~40-55 K (warm dust) and T~20-23 K (cool dust), and with a dust emissivity index epsilon=2. The cool dust can be a major contributor to the FIR emission of starburst galaxies, representing up to 60% of the total flux. This component is heated not only by the general interstellar radiation field, but also by the starburst itself. The cool dust mass is up to ~150 times larger than the warm dust mass, bringing the gas-to-dust ratios of the starbursts in our sample close to Milky Way values, once rescaled for the appropriate metallicity. The ratio between the total dust FIR emission in the range 1-1000 micron and the IRAS FIR emission in the range 40-120 micron is ~1.75, with small variations from galaxy to galaxy. The FIR emission predicted by the dust reddening of the UV-to-nearIR stellar emission is within a factor ~2 of the observed value in individual galaxies and within 20% when averaged over a large sample. If our sample of local starbursts is representative of high-redshift (z>1), UV-bright, star-forming galaxies, these galaxies' FIR emission will be generally undetected in sub-mm surveys, unless (1) their bolometric luminosity is comparable to or larger than that of ultraluminous FIR galaxies and (2) their FIR SED contains a cool dust component.","external_url":"https://arxiv.org/abs/astro-ph/9911459","cited_by_count":5081,"metadata_source":"pith","metadata_fetched_at":"2026-07-10T17:27:26.423607+00:00","pith_arxiv_id":"astro-ph/9911459","created_at":"2026-05-08T17:33:46.963276+00:00","updated_at":"2026-07-11T11:50:26.030339+00:00","title_quality_ok":true,"display_title":"C., Kinney A","render_title":"C., Kinney A"},"hub":{"state":{"work_id":"b47ad93b-b043-4f82-9a7a-7bbd78e9c3d1","tier":"super_hub","tier_reason":"100+ Pith inbound or 10,000+ external citations","pith_inbound_count":140,"external_cited_by_count":5081,"distinct_field_count":4,"first_pith_cited_at":"2016-07-28T17:16:58+00:00","last_pith_cited_at":"2026-07-09T09:07:39+00:00","author_build_status":"needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-08-22T02:59:25.804321+00:00","tier_text":"super_hub"},"tier":"super_hub","role_counts":[{"context_role":"background","n":9},{"context_role":"method","n":4}],"polarity_counts":[{"context_polarity":"background","n":8},{"context_polarity":"use_method","n":4},{"context_polarity":"unclear","n":1}],"runs":{"ask_index":{"job_type":"ask_index","status":"succeeded","result":{"title":"C., Kinney A","claims":[{"claim_text":"(Abridged) We present far-infrared (FIR) photometry at 150 micron and 205 micron of eight low-redshift starburst galaxies obtained with the ISO Photometer. Five of the eight galaxies are detected in both wavebands and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at lambda>40 micron. The FIR spectral energy distributions (SEDs) are best fitted by a combination of two modified Planck functions, with T~40-55 K (warm dust) and T~20-23 K (cool dust), and with a dust emissivity index epsilon=2. The cool dust can be a major contributor to the FIR emiss","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"Since this model excludes scattering, it represents one extreme of the library of dust models, in which the ex- tinction rises exponentially with the dust surface den- sity. 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We first construct a full gas-based attenuation optical depth, τgas(M star)=κ gas Σgas,(16) where the gas surface densityΣgas follows from the gas mass and a size-mass relation defined above andκgas incorporates both the metallicity and dust-to-metal scaling. The gas mass is computed as: Mgas = fg 1−f g M⋆.(17) The gas fraction, f gas, has been shown to be very high (Heintz et al. 2023; Burgarella e","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"In this work, we propose using host galaxies of hydrogen-poor superluminous supernovae (SLSNe-I) as Stellar winds in SLSN hosts3 Table 1.Measured physical properties of the SLSNe and their host galaxies. Object IDz sys M peak g I[O II] IHβ I[O III] IHα EB−V SFRHα 12 + log(O/H) (AB) (cgs) (cgs) (cgs) (cgs) (mag) (M ⊙ yr−1) (dex) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) SN 2020abjc 0.21918−21.09 4.5±0.7 3.0±0.3 10.8±0.5 8.8±0.3 0.03±0.02 0.07±0.01 7.53±0.30 SN 2020zbf 0.19470−20.96 6.1±0.7 1.5±0.3","claim_type":"background","confidence":0.8,"evidence_strength":"citation_context"},{"claim_text":"Before proceeding with the SED fitting analysis, and following the method adopted by the MPA-JHU group, the observed data were corrected for Galactic extinction using the Schlafly & Finkbeiner (2011) dust maps and the O'Donnell (1994) attenuation curve. 14 https://archive.stsci.edu/hlsp/jades 5 2000 4000 6000 8000 Observed Wavelength[Å] 5 10 15 20 25 F [10 17 erg s 1 cm 2 Å 1 ] Local z=0.051 Observed Spectrum Best fit model Observed Photometry 10000 20000 30000 40000 50000 Observed Wavelength[Å]","claim_type":"background","confidence":0.7,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks C., Kinney A because it crossed a citation-hub threshold. 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Five of the eight galaxies are detected in both wavebands and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at lambda>40 micron. The FIR spectral energy distributions (SEDs) are best fitted by a combination of two modified Planck functions, with T~40-55 K (warm dust) and T~20-23 K (cool dust), and with a dust emissivity index epsilon=2. The cool dust can be a major contributor to the FIR emiss","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"Since this model excludes scattering, it represents one extreme of the library of dust models, in which the ex- tinction rises exponentially with the dust surface den- sity. On the other hand, for an internal scattering dust model, the extinction follows: AV,internal =R V × 1.086 k(Hβ)−k(Hα) ×ln γ(Hα) γ(Hβ) (3) γ(λ) = 1−e −τ(λ) τ(λ) (4) τ(λ) = 0.921k(λ) p 1−w(λ) AV,screen RV (5) w(λ) =−0.48 log(λ),(6) withλbeing the wavelength of the line in Angstroms, and again using the standard Milky WayR V o","claim_type":"method","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"shift of observations andz= 20. We force the two first bins to be (0,5) and (5,10) Myr to capture young burst of star-formation. We use a \"bursty continuity\" prior with student t parameters (1,2) following [103]. We use a flat prior for the ionisation parameter (−4<logU <0), a log prior for the metallicity (10 −3 < Z/Z⊙ <2.5). We set an attenuation prior 0< A V <2 using the [104] dust law. 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We first construct a full gas-based attenuation optical depth, τgas(M star)=κ gas Σgas,(16) where the gas surface densityΣgas follows from the gas mass and a size-mass relation defined above andκgas incorporates both the metallicity and dust-to-metal scaling. The gas mass is computed as: Mgas = fg 1−f g M⋆.(17) The gas fraction, f gas, has been shown to be very high (Heintz et al. 2023; Burgarella e","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"In this work, we propose using host galaxies of hydrogen-poor superluminous supernovae (SLSNe-I) as Stellar winds in SLSN hosts3 Table 1.Measured physical properties of the SLSNe and their host galaxies. Object IDz sys M peak g I[O II] IHβ I[O III] IHα EB−V SFRHα 12 + log(O/H) (AB) (cgs) (cgs) (cgs) (cgs) (mag) (M ⊙ yr−1) (dex) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) SN 2020abjc 0.21918−21.09 4.5±0.7 3.0±0.3 10.8±0.5 8.8±0.3 0.03±0.02 0.07±0.01 7.53±0.30 SN 2020zbf 0.19470−20.96 6.1±0.7 1.5±0.3","claim_type":"background","confidence":0.8,"evidence_strength":"citation_context"},{"claim_text":"Before proceeding with the SED fitting analysis, and following the method adopted by the MPA-JHU group, the observed data were corrected for Galactic extinction using the Schlafly & Finkbeiner (2011) dust maps and the O'Donnell (1994) attenuation curve. 14 https://archive.stsci.edu/hlsp/jades 5 2000 4000 6000 8000 Observed Wavelength[Å] 5 10 15 20 25 F [10 17 erg s 1 cm 2 Å 1 ] Local z=0.051 Observed Spectrum Best fit model Observed Photometry 10000 20000 30000 40000 50000 Observed Wavelength[Å]","claim_type":"background","confidence":0.7,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks C., Kinney A because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (8 contexts).","role_counts":[{"n":8,"context_role":"background"},{"n":4,"context_role":"method"}]},"error":null,"updated_at":"2026-06-27T10:05:56.959476+00:00"},"summary_claims":{"job_type":"summary_claims","status":"succeeded","result":{"title":"C., et al","claims":[{"claim_text":"(Abridged) We present far-infrared (FIR) photometry at 150 micron and 205 micron of eight low-redshift starburst galaxies obtained with the ISO Photometer. Five of the eight galaxies are detected in both wavebands and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at lambda>40 micron. The FIR spectral energy distributions (SEDs) are best fitted by a combination of two modified Planck functions, with T~40-55 K (warm dust) and T~20-23 K (cool dust), and with a dust emissivity index epsilon=2. 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