A new luminosity component in 3C 48

Neugebauer, G.; Soifer, B. T.; Miley, G. K.

doi:10.1086/184531

Cited by 26 publications

(17 citation statements)

References 9 publications

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“…The HST images of 3C 48 reveal tidal tails extending for ∼ 35 kpc, confirming previous suggestions of a strong gravitational interaction in this system. Evidence for a massive host was presented earlier from ground-based imaging and spectroscopy Malkan 1984;Stockton & Ridgway 1991), observations of CO (Scoville et al 1993) and far-infrared emission (Neugebauer et al 1985). The host galaxy of 3C 48 has M V = −22.7 mag, brighter than a typical brightest cluster galaxy (M V ≈ − 22.0, Hoessel & Schneider 1985;Postman & Lauer 1995) for Ω 0 = 1.0 and H 0 = 100 km s −1 Mpc −1 , and brighter than any host in the 20 member Local Sample.…”

Section: Nature Of the Hostsmentioning

confidence: 74%

The Host Galaxies of Three Radio‐loud Quasars: 3C 48, 3C 345, and B2 1425+267

Kirhakos

Bahcall

Schneider

et al. 1999

ApJ

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Observations with the Wide-Field/Planetary Camera-2 of the Hubble Space Telescope (HST) are presented for three radio-loud quasars: 3C 48 (z = 0.367), B2 1425+267 (z = 0.366), and 3C 345 (z = 0.594). All three quasars have luminous (∼ 4 × L * ) galaxies as hosts, which are either elliptical (B2 1425+267 and 3C 345) or interacting (3C 48), and all hosts are 0.5 − 1.0 mag bluer in (V − I) than other galaxies with the same overall morphology at similar redshifts to the quasars. The host of 3C 48 has many H II regions and a very extended tidal tail.All nine of the radio-loud quasars studied here and in Bahcall et al. (1997) either have bright elliptical hosts or occur in interacting systems. There is a robust correlation between the radio emission of the quasar and the luminosity of host galaxy; the radio-loud quasars reside in galaxies that are on average ∼ 1 mag brighter than hosts of the radio-quiet quasars.

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Section: Nature Of the Hostsmentioning

confidence: 74%

The Host Galaxies of Three Radio‐loud Quasars: 3C 48, 3C 345, and B2 1425+267

Kirhakos

Bahcall

Schneider

et al. 1999

ApJ

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“…2 for various classes of observed objects, both starbursts and AGN. We select 3C 273 as an example of a powerful quasar, and use the submillimetre data of Neugebauer, Soifer & Miley (1985) in our model; Arp 220 as a starburst using the submillimetre data of Sanders (1999) and the X‐ray data of Iwasawa (1999); and NGC 6240 as a powerful obscured (Compton‐thick) AGN using an estimate of the submillimetre spectrum based on that from Arp 220 normalized by the FIR luminosity and the BeppoSAX spectrum from Vignati et al (1999). We also show how α SX changes as the absorption in NGC 6240 decreases from the measured value of 2×10 24 to 5×10 23 cm −2 and also if the scattered fraction drops to 1 per cent.…”

Section: Discussionmentioning

confidence: 99%

Testing the connection between the X-ray and submillimetre source populations using Chandra

Fabian

Smail

Iwasawa

et al. 2000

Monthly Notices of the Royal Astronomical Society

114

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The powerful combination of the Chandra X‐ray telescope, the SCUBA submillimetre‐wave camera and the gravitational lensing effect of the massive galaxy clusters A2390 and A1835 has been used to place stringent X‐ray flux limits on six faint submillimetre SCUBA sources and deep submillimetre limits on three Chandra sources which lie in fields common to both instruments. One further source is marginally detected in both the X‐ray and submillimetre bands. For all the SCUBA sources our results are consistent with starburst‐dominated emission. For two objects, including SMMJ 14011+0252 at z=2.55, the constraints are strong enough that they can only host powerful active galactic nuclei if they are both Compton‐thick and any scattered X‐ray flux is weak or itself absorbed. The lensing amplification for the sources is in the range 1.5–7, assuming that they lie at z≳1. The brightest detected X‐ray source has a faint extended optical counterpart (I≈22) with colours consistent with a galaxy at z≃1. The X‐ray spectrum of this galaxy is hard, implying strong intrinsic absorption with a column density of about 1023 cm−2 and an intrinsic (unabsorbed) 2–10 keV luminosity of 3×1044 erg s−1. This source is therefore a Type II quasar. The weakest detected X‐ray sources are not detected in Hubble Space Telescope images down to I≃26.

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“…Overplotted are the expected α SX values for 3C273, NGC 6240 ( f sc = 0.05), and Arp 220 (dashed lines); alternative curves for NGC 6240 with less internal absorption (N H = 5 × 10 23 cm 2 ) and a smaller scattered flux fraction ( f sc = 0.01) are also shown (dotted lines). This figure has been adapted from Fabian et al (2000); the references for the 3C273, NGC 6240 and Arp 220 data are Neugebauer, Soifer, & Miley (1985), Iwasawa (1999), Vignati et al (1999), and Sanders (2000). Although five of the X-ray detected submm sources are classified as AGNs, their submm emission is likely to be dominated by star formation.…”

Section: The Origin Of the Submm Emissionmentioning

confidence: 99%

The Chandra Deep Field North Survey. XIV. X-Ray–Detected Obscured AGN[CLC]s[/CLC] and Starburst Galaxies in the Bright Submillimeter Source Population

Alexander¹,

Bauer²,

Brandt³

et al. 2003

The Astronomical Journal

165

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We provide X-ray constraints and perform the first X-ray spectral analyses for bright SCUBA sources ( f 850µm ≥ 5 mJy; S/N≥ 4) in an 8. ′ 4 × 8. ′ 4 area of the 2 Ms Chandra Deep Field-North survey containing the Hubble Deep Field-North. X-ray emission is detected from seven of the ten bright submm sources in this region down to 0.5-8.0 keV fluxes of ≈ 1 × 10 −16 erg cm −2 s −1 , corresponding to an X-ray detected submm source density of 360 +190 −130 deg −2 ; our analyses suggest that this equates to an X-ray detected fraction of the bright submm source population of > ∼ 36%, although systematic effects may be present. Two of the X-ray detected sources have nearby (within 3 ′′ ) X-ray companions, suggesting merging/interacting sources or gravitational lensing effects, and three of the X-ray detected sources lie within the approximate extent of the proto-cluster candidate CXOHDFN J123620.0+621554. Five of the X-ray detected sources have flat effective X-ray spectral slopes (Γ < 1.0), suggesting obscured AGN activity. X-ray spectral analyses suggest that one of these AGNs may be a Compton-thick source; of the other four AGNs, three appear to be Compton-thin sources and one has poor constraints. The rest-frame unabsorbed X-ray luminosities of these AGNs are more consistent with those of Seyfert galaxies than QSOs (i.e., L X ≈ 10 43 -10 44 erg s −1 ). Thus, the low X-ray detection rate of bright submm sources by moderately deep X-ray surveys appears to be due to the relatively low luminosities of the AGNs in these sources rather than Compton-thick absorption. A comparison of these sources to the well-studied heavily obscured AGN NGC 6240 shows that the average AGN contribution is negligible at submm wavelengths. The X-ray properties of the other two X-ray detected sources are consistent with those expected from luminous star formation; however, we cannot rule out the possibility that low-luminosity AGNs are present. The three X-ray undetected sources appear to lie at high redshift (z > 4) and could be either AGNs or starbust galaxies.

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A new luminosity component in 3C 48

Cited by 26 publications

References 9 publications

The Host Galaxies of Three Radio‐loud Quasars: 3C 48, 3C 345, and B2 1425+267

The Host Galaxies of Three Radio‐loud Quasars: 3C 48, 3C 345, and B2 1425+267

Testing the connection between the X-ray and submillimetre source populations using Chandra

The Chandra Deep Field North Survey. XIV. X-Ray–Detected Obscured AGN[CLC]s[/CLC] and Starburst Galaxies in the Bright Submillimeter Source Population

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