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Source WISE Coordinate Redshift L bol a Redshift Reference R.A. (J2000) Decl. (J2000) (10 14 L ☉ ) J000322.91−260316.8 00:03:22.91 −26:03:16.8 4.098 1.6 NED, V10 J001527.40+064012.0 00:15:27.40 +06:40:12.0 3.17 1.2 V10 J004131.50−493612.0 00:41:31.50 −49:36:12.0 3.24 1.8 V10 J010311.30+131618.0 01:03:11.30 +13:16:18.0 2.681 1.6 NED, V10 J012156.04+144823.9 01:21:56.03 +14:48:23.9 2.870 1.1 S10, V10 J012412.47−010049.8 01:24:12.47 −01:00:49.7 2.826 1.0 S10, P12, V10 J013301.90−400628.0 01:33:01.90 −40:06:28.0 3.023 1.0 V10 J015636.00+044528.0 01:56:36.00 +04:45:28.0 2.993 1.0 V10 J020727. 20−374156.0 02:07:27. 20 −37:41:56.0 2.404 1.2 V10 J020950.70−000506.0 02:09:50.71 −00:05:06.4 2.850 1.2 V10, S10, P12 J024008.10−230915.0 02:40:08.10 −23:09:15.0 2.225 1.4 V10 J024854.30+180250.0 02:48:54.30 +18:02:50.0 4.42 1.0 V10 J025240.10−553832.0 02:52:40.10 −55:38:32.0 2.35 1.2 V10 J030722.80−494548.0 03:07:22.80 −49:45:48.0 4.728 1.3 V10 J032108.45+413220.9 03:21:08.45 +41:32:20.8 2.467 1.1 S10.
Figure 3. Normalized rest-frame SEDs of the hyperluminous ( L bol > 10 14 L ☉ ) ELIRG Hot DOGs and optically selected hyperluminous quasars. The SEDs are normalized to the total bolometric luminosity L bol . The shaded region in gray in the upper panel represents the scatter of SEDs for all Hot DOGs with z > 1.6 and L bol > 10 13 L ☉ , while the gray region in the lower panel covers the scatter of SEDs for the hyperluminous quasar sample. The plotted QSO and torus SED models are adopted from Polletta et al. (2006, 2007). The dust model line assumes a dust temperature T d = 450 K with emissivity index β = 2.0. The vertical dashed lines indicate rest-frame wavelengths of 1 and 20 μ m.
0.3 expected from a Kerr black hole. This suggests that the spin of SMBHs in Hot DOGs may be low, perhaps as a result of chaotic accretion due to galaxy merger events.
450 K. If we assume the emitting dust is approximately in thermal equilibrium, the characteristic radius at that temperature is.
The factor τ Salpeter ≡ is the Salpeter (1964) timescale, which describes the time span for an e-fold mass increase of a black hole accreting at its Eddington limit. For a hydrogen-dominated plasma, a 3.3 × 10 4 L ☉ / M ☉ , and with η = 0.057 for a Schwarzschild black hole (Bardeen et al. 1973) rather than the more commonly adopted empirical value of 0.1 (Yu & Tremaine 2002), τ Salpeter is.
1.4–2.4 Gyr. If M seed of the SMBHs in these systems is of order 10–100 M ☉ as suggested by simulations of SMBH seeds from population III stars (Zhang et al. 2008; also see review by Volonteri 2010), the derived time-averaged Eddington ratios of our systems are ( z = 4.6) or.
The photometric measurements used in this paper are listed in Table 2. We include measurements of optical r '-band and selected near-IR bands from ground-based follow-up observations, m >16.
There is the additional possibility that a much larger scale galaxy cluster potential could magnify ELIRGs near a correspondingly larger scale critical curve, which would not necessarily show extreme distortions or local multiple-images, particularly if the sources are quite compact intrinsically. However, the gravitational lensing magnification under this condition is usually small. Although the current optical and near-IR imaging data are not sufficient to fully explore that possibility, the Spitzer data do not show the aggregation of objects within 1' as expected for a massive foreground lensing cluster of galaxies (Assef et al. 2015).
10 8 yr, these high luminosity sources represent the main growth phase for stellar mass if they are powered by starbursts, or of SMBH mass if they are powered by AGNs. From spectroscopic and far-infrared follow-up observations of over 200 Hot DOGs we have identified 20 that meet this L bol threshold. Among these 20 Hot DOGs, 5 have intrinsic L IR ≡ L (rest 8–1000 μ m) > 10 14 L ☉ , an order of magnitude higher than the HyLIRG luminosity threshold. We refer to such systems as "extremely luminous infrared galaxies," or ELIRGs. The rest of our sample has L IR > 5 × 10 13 L ☉ , which should be considered a conservative lower limit due to our luminosity estimate approach (see Section 3.3). For convenience, we refer to these sightly less luminous objects as ELIRGs as well throughout this paper. For comparison, we also present 116 optically selected quasars from the literature with L bol > 10 14 L ☉ .
We then visually inspected the SEDs and images of.
4.6.2. Time-averaged Eddington Ratios and Radiation Efficiency.
Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available.
Figure 4. Luminosity histogram of L bol > 10 14 L ☉ WISE Hot DOGs (in red) and optically selected quasars (in black). There are 20 Hot DOGs and 116 quasars in this plot.
450 K, as shown in the upper panel of Figure 3. This suggested temperature does not imply a single-temperature dust system, but is rather a characteristic temperature for the hot dust emission component. Further discussion of the SEDs and implied dust temperatures is included in Section 4.3.
0.2 for an intermediate spinning black hole, and η.
We present the sample and m >−1 Mpc −1 , Ω m = 0.3, and Ω Λ = 0.7.
The WISE ELIRGs presented in this paper are from the subset of Hot DOGs selected from the WISE All-Sky Source Catalog (Cutri et al. 2012) with spectroscopic redshifts (P. R. M. Eisenhardt et al. 2015, in preparation) and far-infrared photometry. The redshift and L bol distribution of the current Hot DOG sample is shown in Figure 1. The sample of 20 Hot DOGs with L bol ≥ 10 14 L ☉ corresponds to approximately 15% of the current sample with spectroscopic redshifts and multi-wavelength follow-up observations. The coordinates and redshifts of the 20 sources are listed in Table 1. The redshift quality flag "A" in Table 1 indicates unambiguous redshift typically determined from multiple emission or absorption features. The flag "B" signifies a less secure redshift determined from a robustly detected line but with uncertain >
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
where ( z ) is the Eddington ratio.
, Roberto J. Assef 3 , Andrew W. Blain 4 , Carrie R. Bridge 5 , Dominic J. Benford 6 , Roc M. Cutri 7 , Roger L. Griffith 8 , Thomas H. Jarrett 9 , Carol J. Lonsdale 10 , Frank J. Masci 7 , Leonidas A. Moustakas 1 , Sara M. Petty 11 , Jack Sayers 5 , S. Adam Stanford 12 , Edward L. Wright 2 , Lin Yan 7 , David T. Leisawitz 6 , Fengchuan Liu 1 , Amy K. Mainzer 1 , Ian S. McLean 2 , Deborah L. Padgett 6 , Michael F. Skrutskie 13 , Christopher R. Gelino 7 , Charles A. Beichman 7 , and Stéphanie Juneau 14.
20 and redshift z . Thus, from Equation (4), we derive that the evolution of black hole mass M BH can be written as.
The far-IR and submillimeter photometry of the WISE selected ELIRGs, listed in Table 2, was acquired with Herschel . The Herschel data (PI: P. Eisenhardt, Proposal >hipe v11.1.0. For W0831+0140, which was not included in the Herschel program but was covered by the Herschel ATLAS survey (Eales et al. 2010), the far-IR photometry was taken from the public Herschel archive.
Table 3. Properties of Optically Selected Quasars with L bol > 10 14 L ☉
0.1, a commonly adopted value for a slowly spinning or non-spinning black hole, η.
2.5, for a source at z = 3.2 (the median ELIRG redshift), and the value of θ E versus W 1 for a lens at this redshift is shown by the solid blue line. Neighboring objects must be above this line to produce high magnification of the Hot DOG. No source falls above the line, and only one comes close. At the observed separations of W 1 objects in the ELIRG fields, such objects would need masses well above 10 14 M ☉ .
4. DISCUSSION.
a See Section 3.3 for definition.
3. Thus, the use of single-wavelength ν L ν values such as L 5.8 μ m and L 7.8 μ m to represent L bol needs to be reevaluated considering dust obscuration and thermal dust emission.
L 1−20 μ m , or L MIR as shown in Figure 8, is a better indicator of the hot dust-dominated luminosity of these hyperluminous systems, in contrast to the traditional infrared luminosity L IR value which is more sensitive to diffuse dust emission powered by a starburst. As shown in Table 5, L MIR > L >20 μ m for every ELIRG. The bolometric contribution of emission blueward of 1 μ m is negligible for the Hot DOGs and is likely redistributed by dust to rest-frame mid-IR wavelengths, resulting in the high L MIR / L bol.
3 (Kelly & Shen 2013), though Hot DOGs could be in a different accretion phase from Type 1 quasars.
7 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA.
Chao-Wei Tsai et al 2015 ApJ 805 90.
1500 K. Here we assume that the bolometric luminosity is equal to the dust absorbed UV luminosity in these highly obscured systems. Unlike optically selected quasars, in which the variation timescale of optical emission is much shorter because the optical light comes directly from smaller physical scales (Schmidt 1963), the fluctuations of luminosity over time in Hot DOGs will be smoothed out by radiation reprocessing by the dust. The 16 pc diameter of the sublimation region sets the shortest variation timescale to be.
5 Division of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA.
450 K is responsible for the high luminosities. These galaxies are likely powered by highly obscured active galactic nuclei (AGNs), and there is no evidence suggesting these systems are beamed or lensed. We compare this WISE -selected sample with 116 optically selected quasars that reach the same L bol level, corresponding to the most luminous unobscured quasars in the literature. We find that the rest-frame 5.8 and 7.8 μ m luminosities of the WISE -selected ELIRGs can be 30%–80% higher than that of the unobscured quasars. The existence of AGNs with L bol > 10 14 L ☉ at z > 3 suggests that these supermassive black holes are born with large mass, or have very rapid mass assembly. For black hole seed masses.
1 (see discussion of Section 4.6.1). The age of the universe at that redshift is.
By selection, optical quasars have relatively low extinction at visible wavelengths, suggesting that feedback to the ambient material may have cleared out the surrounding dust cocoon and terminated further accretion or star formation in the inner regions of the host galaxy. Several lines of evidence suggest that quasars must have spent significant time growing in the obscured phase (Kelly et al. 2010; Assef et al. 2015), and the 20–30 keV peak of the cosmic X-ray background implies that most black hole growth is obscured (Gilli et al. 2007). Key open questions for understanding quasar evolution include: What was the SMBH activity just prior to the quasar "blowout" phase, when the SMBH was still highly embedded in dust and gas from the parent galaxy coalescence event? Were the SMBHs accreting as rapidly as optical quasars, faster than quasars because of the infalling material, or was the accretion suppressed by the dynamical interaction? Answers to these questions may be hidden in highly obscured, but still powerful quasars.
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The previous section discusses a simple model of M BH growth history (Equation (6)) in which the variables are the seed black hole mass M seed , the radiative efficiency η , and the Eddington ratio ( z ). Current models suggest seed black hole masses ranging from.
3.3. Luminosity Estimates.
The minimum lifetime of the high luminosity phase in hyperluminous Hot DOGs can be estimated by considering the depletion time of the observed dusty material. The peak of the ELIRG SEDs suggests that the luminosity is dominated by radiation from hot dust at T d.
The SEDs of the quasars do not extend to rest frame wavelengths >8 μ m due to a lack of comprehensive far-IR data. The contribution to the bolometric luminosity at longer wavelengths is expected to be 20 μ m , respectively. For simplicity, we refer to L 1–20 μ m as L MIR hereafter. The L >20 μ m should be distinguished from infrared luminosity, L IR , which is defined as the accumulated luminosity between 8–1000 μ m, and from the traditional far-infrared luminosity, L FIR , which covers emission from 40 to 500 μ m. The results are listed in Table 5.
65% (median value). In optically selected populations, especially the high luminosity quasars, L MIR contributes only.
We have also examined all of our 2D spectra. We have closely examined the four cases (W1248–2154, W2042–3245, W2246–0526, and W2246–7143) where nearby objects appear in the data (P. R. M. Eisenhardt et al. 2015, in preparation). Other than W1248–2154, discussed below, we have not identified any cases of two different redshifts superimposed that might be indicative of strong lensing (e.g., SLACS survey sample; Bolton et al. 2004, 2006). As discussed in detail below, we conclude that gravitational lensing is not causing the high luminosity of W1248–2154.
4.6.3. Seed Black Hole Mass and Black Hole Spin.
Figure 6. Mass limit of unresolved lenses vs. redshift, assuming a source at z = 3.2. The blue curve shows the upper limit due to the brightest W 1 photometry ( W 1 = 16.8) observed for ELIRGs. The red-orange and magenta curves show the 3- σ detection limit of our high resolution imaging with HST WFC3 in F160W, and Keck NIRC2 with AO in the K -band. These curves are calculated using elliptical galaxy SED template from Polletta et al. (2007) with assumption of M / L B.
Figure 1. The redshift and bolometric luminosity, L bol , of WISE Hot DOGs at 1 10 14 L ☉ threshold, shown by the horizontal dashed line.
Published 2015 May 22 • © 2015. The American Astronomical Society. All rights reserved. The Astrophysical Journal , Volume 805 , Number 2.
We can also relate the observed luminosity to the Eddington luminosity,
4.8. A Luminosity Limit at ?
2 × 10 5 L ☉ for the Lyman continuum photon rate N Lyc = 10 49 s −1 derived from radio measurements. If the obscured starburst case applies to the hyperluminous Hot DOGs, 10 14 L ☉ would correspond to N Lyc.
40 pc, contains 2700 M ☉ . Because of its physical size, we expect that large flux variations in these Hot DOGs should not occur on timescales 200 yr.
The ELIRG Hot DOG systems are at z > 2.5, leaving the SMBHs in them black hole mass growth rate and radiative efficiency η ( z ), the observed luminosity at redshift z is.
The m >17 The anticipated color difference in between IRAC [4.5] and WISE [4.6] is less than 0.1 magnitude, or about 10% in flux density, thus no color correction has been applied for that band.
14 CEA-Saclay, DSM/IRFU/SAp, F-91191 Gif-sur-Yvette, France.
10 12 M ☉ if the host galaxies follow the M– σ correlation, comparable to local giant elliptical galaxies in clusters. If ( z ) 10 M ☉ , larger than the most massive SMBHs known in the local universe (McConnell et al. 2011). The lack of such massive black holes at the present epoch is not easy to explain when the abundance of Hot DOGs matches that of powerful quasars (Assef et al. 2015), whose abundance is in turn consistent with the distribution of large elliptical galaxies today. Furthermore, if M BH > 10 10 M ☉ for Hot DOGs, we would expect more massive host galaxies than observed unless Hot DOGs deviate substantially from the empirical M – σ relation (Assef et al. 2015). While the extremely massive black holes and galaxy hosts expected for ELIRGs with low Eddington ratios are not found, there is some evidence that Hot DOGs are in rich environments. Follow-up observations using the SCUBA-II camera on JCMT show enhanced numbers of 850 μ m continuum sources within 1 5 of Hot DOGs (Jones et al. 2014), and Spitzer IRAC images also show enhanced densities of sources with red IRAC colors ([3.6] − [4.5] > 0.37), indicative of galaxies at z 1 (Assef et al. 2015).
If Hot DOGs are accreting below the Eddington limit the SMBH masses for ELIRGs are >3 × 10 9 M ☉ . This implies stellar masses.
15 NASA Postdoctoral Program Fellow.
0 14. The red cross shows the position of W1248-2154 from the AllWISE Catalog and the 0 32 uncertainty, which includes 0 2 registration uncertainty (1 σ ) of the K -band image and the.
Figure 11. Upper limits on radiative efficiency implied by hyperluminous Hot DOGs, quasars, and high redshift ( z > 6) quasars (color coded as in Figure 10). Black holes radiating too high a fraction of their accreted mass cannot grow large enough to produce the observed luminosities at the Eddington limit. The filled circles and magenta lines show cases with initial black hole seed mass M seed = 10 3 M ☉ , and open circles and yellow lines show M seed = 10 6 M ☉ . The dashed lines outline the luminosity threshold of L bol > 10 14 L ☉ used in this paper. The horizontal dotted lines are the theoretically predicted radiative efficiency of a non-spinning black hole ( η = 0.057) and a highly spinning black hole ( η = 0.32). All the lines and dots are plotted assuming a constant Eddington ratio = 1.
Source WISE Coordinates z Q z R.A. (J2000) Decl. (J2000) W0116−0505 01:16:01.42 −05:05:04.2 3.173 a A W0126−0529 01:26:11.96 −05:29:09.6 2.937 B W0134−2922 01:34:35.71 −29:22:45.4 3.047 A W0149+2350 01:49:46.18 +23:50:14.6 3.228 A W0220+0137 02:20:52.13 +01:37:11.4 3.122 a A W0255+3345 02:55:34.90 +33:45:57.8 2.668 A W0410−0913 04:10:10.61 −09:13:05.2 3.592 a A W0533−3401 05:33:58.44 −34:01:34.5 2.904 A W0615−5716 06:15:11.07 −57:16:14.6 3.399 B W0831+0140 08:31:53.26 +01:40:10.8 3.888 A W0859+4823 08:59:29.93 +48:23:02.0 3.245 a A W1248−2154 12:48:15.21 −21:54:20.4 3.318 A W1322−0328 13:22:32.57 −03:28:42.2 3.043 A W1838+3429 18:38:09.16 +34:29:25.9 3.205 B W2042−3245 20:42:49.28 −32:45:17.9 3.963 B W2201+0226 22:01:23.39 +02:26:21.8 2.877 A W2210−3507 22:10:11.87 −35:07:20.0 2.814 B W2246−0526 22:46:07.57 −05:26:35.0 4.593 A W2246−7143 22:46:12.07 −71:44:01.3 3.458 A W2305−0039 23:05:25.88 −00:39:25.7 3.106 A.
where z is the Eddington ratio, and a is a constant associated with the opacity of accreting materials. By combining Equations (2) and (3) with cosmic time t ( z ), one can derive.
450 K contributes the majority of the luminosity. This dust component, with a characteristic radius of.
Source r '-band 3.6 μ m 4.5 μ m 12 μ m 22 μ m 70 μ m 160 μ m 250 μ m 350 μ m 500 μ m ( μ Jy) ( μ Jy) ( μ Jy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) W0116−0505 10.2(0.5) 51(2) 89(1) 2.4(0.2) 12.1(1.1) 50(3) 93(6) 42(11) b 99(11) b 5.0(0.2) 19.7(1.4) 36(3) 40(6) 46(12) 41(10) 50(11) W0149+2350 a 25(2) 38(1) 2.0(0.1) 12.4(1.0) 55(3) 120(6) 64(10) 56(11) a 39(6) b 36(10) b 2.3(0.2) 16.5(1.2) 86(2) 73(7) 52(10) 42(10) a 27(2) 46(1) 2.9(0.2) 13.4(1.2) 28(3) 110(6) 122(10) 117(11) 97(15) W0533−3401 7.0(0.2) a 36(2) 73(1) 3.2(0.1) 12.0(1.0) 39(2) 98(10) 124(10) 85(10) 50(15) W0615−5716 ⋯ 32(2) 49(1) 2.4(0.1) 15.0(0.8) 58(3) 110(6) 53(10) 37(11) a 31(8) b 63(11) b 2.8(0.2) 10.3(1.1) a 16(2) 45(1) 2.6(0.2) 12.2(1.3) 29(3) 63(10) 55(10) 57(11) 48(14) W1248−2154 2.7(0.2) a 46(5) b 36(10) b 2.8(0.1) 13.1(0.9) 37(3) 67(2) 53(11) 36(10) a 29(2) 60(1) 2.5(0.1) 11.5(1.1) 47(3) 64(7) 67(10) 47(11) a 15(2) 19(1) 2.7(0.2) 16.4(1.3) 20(3) 30(5) 44(10) a 42(8) b 92(11) b 4.9(0.2) 18.1(1.4) 27(3) 141(7) 135(11) 138(12) 82(15) W2210−3507 1.3(0.1) a 32(6) b 36(12) b 2.3(0.1) 16.5(1.0) 51(3) 140(6) 86(10) 95(11) 77(15) W2246−0526 b 17(6) b 1.4(0.1) 12.6(1.0) 29(3) 87(6) 71(9) 62(11) 31(15) W2305−0039 0.6(0.2) a 58(6) b 67(11) b 3.4(0.2) 24.6(1.4) ⋯ ⋯ 83(10) 59(11) 44(15)
10 14.5 L ☉ of W2246–0526 exceeds the most luminous quasars listed in Table 3 (see Figure 4). Could there be even more luminous Hot DOGs?
Figure 9. Ratio of L 5.8 μ m to L bol ( left ) and L 7.8 μ m to L bol ( right ) of hyperluminous Hot DOGs and quasars. The dashed lines represent the median values of luminosity ratios for Hot DOGs (red) and quasars (blue). The hatched regions show a 1 σ range from the median value.
5. Thus far, we have not observed any system at that L bol level. Such systems are expected to be rare: no more than a few over the whole sky based on the luminosity function of Hot DOGs and optical quasars. At z > 5, the hot dust emission peak at 6 μ m will shift to.
8 Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA.
a Ground-based r '-band photometry from P. R. M. Eisenhardt et al. (2015, in preparation). b Data from WISE 3.4 or 4.6 μ m measurements.
To ensure that the intrinsic luminosities of the optically selected quasars are greater than the 10 14 L ☉ threshold, we removed known gravitationally lensed systems and blazars. We invoked the catalog of strong gravitational lensing systems from "the Master Lens Database" 18 (L. A. Moustakas et al. 2015, in preparation), and the list of blazars from "the Roma-BZCAT Multi-frequency Catalogue of Blazars" (Massaro et al. 2009) version 4.1.1—2012 August). Of the 140 luminous quasars, 9 are in known strong gravitational lensing systems, and 15 are known blazars. This leaves a total of 116 hyperluminous quasars with L bol > 10 14 L ☉ , including 68 quasars from the SDSS DR7 quasar search (Schneider et al. 2010). These quasars are listed in Table 3.
5. SUMMARY.
We estimate a dust sublimation radius (Barvainis 1987) of.
Case 2 is addressed in Figure 6, which shows the lens mass versus redshift for a source at z = 3.2, the median redshift of the ELIRGs. In this case the lens would need to have W 1 > 16.8 (or 12 M ☉ lenses up to z = 1.5, assuming M / L B.
Note added in proof . After this paper was submitted, we were alerted to the discovery of SDSS J0010+2802 at z = 6.3 with M BH.
5. Lower mass lenses are possible, of course, but they must reach the critical mass surface density for gravitational lensing (see e.g., Subramanian & Cowling 1986). The remaining parameter space is highlighted as the gray shaded region in Figure 6. This parameter space can be investigated where we have high-resolution near-IR imaging.
3 Núcleo de Astronomía de la Facultad deIngeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile.
Table 1. Properties of WISE ELIRGs.
THE MOST LUMINOUS GALAXIES DISCOVERED BY WISE.
3–5 lower without any consideration of selection effects. Assef et al. (2015) find that the space density of ELIRG Hot DOGs is comparable to the space density of extremely luminous unobscured quasars from SDSS-III BOSS (Ross et al. 2013) after correcting for the selection function used to identify Hot DOGs from WISE photometry and for spectroscopic incompleteness.
5 in solar units (e.g., Faber & Gallagher 1979; Napolitano et al. 2005) to show the relationship between θ E , W 1 photometry, and the mass of the lens. The maximum θ E occurs near a lens redshift.
10 51 erg). Rowan-Robinson (2000) argues that a starburst component is necessary for explaining the far-IR and submillimeter ( λ ≥ 50 μ m) SEDs of HyLIRGs. Could an extreme starburst provide this much energy for ELIRGs?
The SEDs of the WISE -selected ELIRGs are shown in Figure 3, normalized by the integrated luminosity over the plotted SEDs. The SEDs of the L bol ≥ 10 14 L ☉ Hot DOGs are similar to those of their less luminous siblings, which are outlined by the shaded region. The steep rise from rest frame 1–4 μ m reflects the selection criteria. These SEDs do not match empirical starburst or dusty AGN templates, although they are close to the torus model of Polletta et al. (2006). However, they are steeper than the torus model at λ 60 μ m. The rest-frame flux density peak is at shorter wavelengths than the peak of the dusty starburst system Arp 220, which is at about 60 μ m. This indicates emission from hotter dust in these WISE -selected hyperluminous galaxies. The emission excess around rest frame 6 μ m can be explained by dust emission T d.
2. SAMPLE AND OBSERVATIONS.
10 M ☉ from simulations of the end products of population III stars (e.g., Zhang et al. 2008) to.
Hyperluminous infrared galaxies (Cutri et al. 1994), or HyLIRGs, are galaxies whose infrared luminosity ( L IR ) exceeds 10 13 L ☉ (Sanders & Mirabel 1996). They have generally been discovered due to their substantial IR emission from far-IR surveys such as those with the Infrared Astronomical Satellite ( IRAS ; Neugebauer et al. 1984), the Submillimeter Common-User Bolometer Array (SCUBA) at James Clerk Maxwell Telescope, or, more recently, the Herschel Space Telescope (Cutri et al. 1994; Frayer et al. 1998; Rowan-Robinson 2000, and references therein; Casey et al. 2012b). Infrared emission dominates the energy output of these hyperluminous systems, so their L IR is approximately equal to their bolometric luminosity L bol . Galaxies with such high luminosity, usually powered by active galactic nucleus (AGN; Weedman et al. 2012), intense starbursts (Rowan-Robinson 2000), or a mixture of both, represent a rapid growth phase of the supermassive black holes (SMBHs) and/or the stellar mass portfolio of the host galaxies. It has been suggested that this phase at 1 10 14 L ☉ ), such as S5 0014+81 (Osmer et al. 1994), SDSS J1701+6412 (Hewett & Wild 2010), and HS 1946+7658 (Lu et al. 1996). These quasars have SMBH masses of.
Chao-Wei Tsai 1,15 , Peter R. M. Eisenhardt 1 , Jingwen Wu 2 , Daniel Stern 1.
We present 20 Wide-field Infrared Survey Explorer ( WISE )-selected galaxies with bolometric luminosities L bol > 10 14 L ☉ , including five with infrared luminosities L IR ≡ L (rest 8–1000 μ m) > 10 14 L ☉ . These "extremely luminous infrared galaxies," or ELIRGs, were discovered using the " W 1 W 2-dropout" selection criteria which requires marginal or non-detections at 3.4 and 4.6 μ m ( W 1 and W 2, respectively) but strong detections at 12 and 22 μ m in the WISE survey. Their spectral energy distributions are dominated by emission at rest-frame 4–10 μ m, suggesting that hot dust with T d.
20), so the maximum possible T age would decrease by less than 0.15. Differences in τ Salpeter will affect . The higher η of rap > . The same arguments apply to the ELIRG quasars in the same redshift range. Thus, the time-averaged Eddington ratios of the ELIRG systems we discuss here are securely larger than 25%. In comparison, the most massive black hole known so far with.
Note. The numbers in parentheses are the 1– σ uncertainty in photometry. The upper limits are at 3 σ .
0 14. The final NIRC2 image was registered to the seeing-limited J -band image from Assef et al. (2015), which has its WCS matched to the AllWISE WCS using W 1 sources in the field of view.
Figure 9 shows ν L ν at 5.8 μ m ( L 5.8 μ m ) and 7.8 μ m ( L 7.8 μ m ), which have often been used to characterize AGN luminosities in the literature (e.g., Weedman et al. 2012). Common practice is to interpolate the SED to obtain these numbers, or to estimate them from an SED model. These numbers are convenient for statistical analyses such as deriving the quasar luminosity function. However, these monochromatic luminosities do not capture the variation in dust temperature distribution in different AGNs, which could be dramatic in obscured systems such as Hot DOGs. The ratios of L 5.8 μ m / L bol and L 7.8 μ m / L bol are substantially offset between ELIRG quasars and ELIRG Hot DOGs, and the scatter is large for both populations, particularly for quasars. The conversion from these monochromatic values to total L bol can vary by a factor of.
13 Department of Astronomy, University of Virginia, Charlottesville, VA 22903, USA.
8 × 10 13 L ☉ is on the order of 2700 M ☉ . This dust mass is just.
Another possible explanation for the high luminosity of Hot DOGs is gravitational lensing by massive foreground systems. The most luminous known quasars, J0831+5245 and with apparent L bol 10 15 L ☉ , are both gravitationally lensed (Lawrence et al. 1992; Patnaik et al. 1992; Irwin et al. 1998). For the WISE ELIRGs, while we cannot completely rule out the lensing hypothesis for these hyperluminous Hot DOGs, we consider the likelihood of strong lensing to be small based on the following arguments.
We report 20 highly obscured, ELIRG AGNs discovered by WISE . These sources, because of their similarity to DOGs with steeply rising SEDs toward the mid-IR albeit with hotter dust components, have been dubbed Hot DOGs by Wu et al. (2012). The luminosities of these objects exceed 10 14 L ☉ , making them among the most luminous (non-transient) systems in the universe. They are not likely to be powered by starbursts, but rather by highly obscured and actively accreting AGNs. Based on their lack of variability and the absence of evidence for foreground lensing systems in their spectra and images, we conclude that the high luminosity is generally not a result of relativistic beaming or gravitational lensing.
3 × 10 10 M ☉ at z > 2 (Kelly et al. 2010) in the broad-line QSO phase. The discovery of hyper-luminous quasars at z > 6 (Fan et al. 2001) further suggests that SMBHs can grow to 10 9 M ☉ (Barth et al. 2003; Willott et al. 2005; Mortlock et al. 2011) by the time the universe is only.
4.2.1. W1248–2154.
1.2 × 10 14 L ☉ based on an SED model with T dust = 98 K. It is the brightest object in their sample, and tentatively classified as a starburst system based on its optical spectrum (Casey et al. 2012a). Our conservative estimate using WISE and Herschel photometry would imply its L bol is.
The luminosity distributions of hyperluminous Hot DOGs and quasars are shown in Figure 4. The 20 luminous Hot DOGs have luminosities up to 10 14.6 L ☉ , reaching the same level as the non-lensed quasars, although the numbers are a factor of.
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3 × 10 9 M ☉ SMBHs accreting near the Eddington limit. Their existence at redshift 2.8 25% up to their observed epochs. It would be difficult for these SMBHs to grow to 10 9 M ☉ with the relatively high radiative efficiency.
Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available.
450 K. The SED becomes Rayleigh–Jeans around 40–60 μ m, corresponding to T d.
1 Gyr old. The existence of such luminous quasars at early times constrains SMBH seed masses and their growth history (Volonteri & Rees 2006), implying a high accretion rate at high redshift, rather than slower accretion over a Hubble time (Hopkins et al. 2006b).
The WISE mid-IR color–color diagram at [3.4], [4.6], and [12] is shown in Figure 2. The WISE -selected ELIRG Hot DOGs occupy a wider range of [3.4]–[4.6] color than do the hyperluminous quasars, and the Hot DOGs are.
6 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
2.3. Extremely Luminous Optically Selected Quasars from the Literature.
450 K. At that temperature, the required dust mass to produce the observed L MIR.
Are there other infrared objects, either starbursts or obscured AGNs, with similarly high luminosities? Recently, 1HERMES X24 J161506.65+543846.9 at z = 4.952 was discovered by Herschel HerMES survey (Casey et al. 2012a). Its L IR is reported to be.
The authors thank the anonymous referee for the constructive comments and for encouraging a more thorough discussion of gravitational lensing in this paper. This publication makes use of data products from the Wide-field Infrared Survey Explorer , which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE , which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. This work is also based in part on observations made with the Spitzer Space Telescope , which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. Part of this research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive and the NASA/IPAC Extragalactic Database (NED), which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contracts with the National Aeronautics and Space Administration. This material is based upon work supported by the National Aeronautics and Space Administration under Proposal No. 13-ADAP13-0092 issued through the Astrophysics Data Analysis Program. C.-W.T. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. R. J. A. was supported by Gemini-CONICYT grant number 32120009.
10 3 M ☉ , we expect that SMBHs have radiative efficiency on average lower than 15% to form the ELIRGs and hyperluminous quasars at z > 4. If a higher seed mass is adopted, the upper limits of η are still 7), (2) experience substantial super-Eddington accretion episodes in their growth history (Kelly & Shen 2013), or (3) have sustained lower radiation feedback to accretion due to lower radiation efficiency for slowly spinning black holes. In the latter case, some mechanism, such as accretion with randomized directions (King & Pringle 2006; King et al. 2008; Fanidakis et al. 2012), has to interrupt the increase of black hole spin by angular momentum transported from a regulated accretion disk, otherwise a black hole can be spun up close to the theoretical limit over a few Salpeter timescales.
4.6. Black Hole Mass and Accretion History.
1. INTRODUCTION.
1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA.
Note. The bolometric luminosity L bol is conservatively estimated using power laws to interpolate over photometry from the r '-band to Herschel SPIRE [500] μ m if applicable. See Section 3.3 for details. L IR is the conventional infrared luminosity from rest-frame 8–1000 μ m. L 0.1–1 μ m is the luminosity from rest-frame 0.1–1 μ m. L 1–20 μ m , which is also refered as L MIR in this paper, covers 1–20 μ m. L >20 μ m is the luminosity at wavelengths longer than 20 μ m. L 5.8 μ m and L 7.8 μ m are the monochromatic luminosities at rest-frame 5.8 and 7.8 μ m, respectively, estimated by interpolating the SEDs.
We present the full SED of these objects from observed optical to far-IR wavelengths. For both hyperluminous Hot DOGs and unobscured quasars of similarly high luminosity, we show that the conversion from monochromatic mid-IR luminosity to total L bol can vary by a factor of.
Our systematic search for ELIRGs using the " W 1 W 2-dropout" selection criteria has identified about 1000 candidates in the WISE database (Eisenhardt et al. 2012). Among the 150 of these candidates from which we have redshift information, a total of 20 ELIRGs at z > 2.5 have been discovered as reported in this paper, including the most luminous system, W2246–0526 at z = 4.593 with L bol.
1 kpc and surface mass density Σ equals to Σ CR , the critical surface mass density necessary for gravitational lensing. The shaded region indicates the remaining lens galaxy mass parameter space.
Figure 7. A 5'' × 5'' subsection of the Keck NIRC2 image of W1248–2154 in the K -band. The PSF FWHM is.
At high Eddington rates, the black hole mass in ELIRGs can grow by an order of magnitude over 10 7 yr, much faster than the growth of stellar bulges. The relatively tight M – σ relation seen in the local universe suggests that high Eddington rate phases do not account for a significant fraction of cosmic SMBH mass growth.
Facilities: WISE - Wide-field Infrared Survey Explorer, Spitzer (IRAC) - Spitzer Space Telescope satellite, Herschel (PACS, SPIRE) - European Space Agency's Herschel space observatory, Keck:II (NIRC2) -
11 Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA.
few × 10 9 M ☉ or higher, if they are emitting at or close to the Eddington limit. At the Eddington limit, SMBH mass grows on the Salpeter e -folding time scale of 45 Myr (Salpeter 1964), and the most massive SMBHs can reach.
Figure 8. Normalized histogram of L MIR / L bol for WISE Hot DOGs and optically selected quasars with L bol > 10 14 L ☉ , where L bol is the total integrated luminosity calculated using power-law-connected SEDs and L MIR is the integrated luminosity from 1 to 20 μ m.
20 (Couchman & Rees 1986; Bromm et al. 2009), the age of the black holes since their appearance is , and the time-averaged Eddington ratio is.
Without obvious starburst examples in the ELIRG luminosity range, we consider He 2–10, a local dwarf galaxy and a highly obscured starburst system, as an analogy to evaluate the possibility that the high luminosity is supported by star formation. In He 2–10, compact starburst regions are highly obscured and show mid-IR emission from hot dust (Beck et al. 2001). Beck et al. (2001) estimate an infrared luminosity L IR.
The Hot DOG SEDs generally peak between rest-frame 4 and 10 μ m (see Figure 3), suggesting that the emitting dust can have temperatures up to T d.

The red cross in Figure 7 shows the AllWISE position of W1248–2154, which has an uncertainty of 0 25. The 0 2 extent of the cross indicates the astrometric uncertainty of the K -band image with respect to the AllWISE coordinate system. We do not find any significant gravitational lensing signatures in this image. We s K -band magnitude of.
3. RESULTS AND ANALYSES.
10 3 M ☉ , either sustained super-Eddington accretion is needed, or the radiative efficiency must be BibTeX RIS.
5. If so, this might explain the upper luminosity bound at 10 14.5 L ☉ for hyperluminous Hot DOGs and quasars in Figure 10.
4.3. Dust Temperatures and SED Components.
4 Department of Physics & Astronomy, University of Leicester, 1 University Road, Leicester, LE1 7RH, UK.
As a comparison sample, we identified known quasars with L bol > 10 14 L ☉ from the following large-scale quasar catalogs: (i) the 13th edition of the Catalogue of Quasars and Active Nuclei (Véron-Cetty & Véron 2010), (ii) the 2dF QSO Redshift Survey (Croom et al. 2004), (iii) the 2dF-SDSS LRG and QSO Survey (Croom et al. 2009), (iv) the SDSS Quasar Catalog V from the 7th SDSS data release (Schneider et al. 2010), and (v) the Sloan Digital Sky Survey (SDSS) Quasar Catalog from SDSS 9th data release (Pâris et al. 2012). In addition, we considered objects with the spectroscopic class of "QSO" in the SDSS 10th Data Release (DR10; Ahn et al. 2013). For the luminous SDSS DR10 quasar sample, we visually checked for mis-identified spectral features or artifacts. We also included 46 objects that are listed as "HyLIRGs" in the NASA/IPAC Extragalactic Database (2013 August 27th version). We utilized the redshift information of quasars reported in these catalogs, and estimated their bolometric luminosities using photometric data from GALEX GR7 (Martin et al. 2005), SuperCosmos (Hambly et al. 2001), SDSS DR10 (Ahn et al. 2013), 2MASS (Skrutskie et al. 2006), UKIDSS DR9 (Lawrence et al. 2007), the AllWISE Data Release (Cutri et al. 2013), IRAS (Neugebauer et al. 1984), and Akari (Murakami et al. 2007).
4.2. Possible Effects of Lensing?
Note. The WISE coordinates are from the AllWISE database. The " Q z " flag indicates the quality of the redshift (see Section 2 for details).
Like quasars, Hot DOGs are likely powered by efficiently accreting SMBHs, albeit with extremely high obscurations. Here we consider the constraints on the mass and growth history of the SMBHs in the extremely luminous Hot DOGs and quasars based on their luminosities and redshifts. Below we show that the existence of ELIRGs at z > 3 implies SMBHs in ELIRGs have (1) a seed mass 10 3 M ☉ ; (2) a sustained super-Eddington accretion phase; or (3) a sustained radiation efficiency of.
Among the optical spectra of all 20 ELIRGs, only W1248–2154 suggests lensing. The spectrum of W1248–2154 shows two sources at z = 0.339 and z = 3.326 separated by 1 3 (P. R. M. Eisenhardt et al. 2015, in preparation). To explore the lensing hypothesis, we obtained K -band images of W1248–2154 using the NIRC2 camera with the Laser Gu per frame and pixel scale of 0 0397/pixel. Thirty K -band images (120 sec per image) were obtained using a three-position dither pattern that avoided the noisy, lower-left quadrant. The total effective exposure time was 60 minutes.
1% of their lifetime in a luminous, high accretion rate mode, and 99% in a dim, low accretion phase (Hopkins et al. 2006b). The high accretion phase dominates the BH mass growth. For ELIRGs, the accretion rate required to radiate at the ELIRG luminosity level is . For the typical η = 0.1 radiative efficiency of a slow-spinning black hole,
The extremely red SEDs of Hot DOGs suggests the extinction toward their central AGNs is very high, reaching A V 30 mag (Eisenhardt et al. 2012; Assef et al. 2015; Stern et al. 2014). The absorbed energy is released at mid-IR wavelengths via thermal dust emission. As discussed in the previous two sections, the reprocessed energy ( L MIR ) output in hyperluminous Hot DOGs dominates the total luminosity, and matches the luminosity emitted directly from the accretion disk ( L 0.1–1 μ m ) in optically selected hyperluminous quasars. This enormous thermal dust luminosity suggests a dust covering fraction close to unity, rather than an edge-on dusty torus.
Figure 10. Bolometric luminosity L bol vs. redshift. The age of the SMBH since formation at z.
12 Department of Physics, University of California Davis, One Shields Avenue, Davis, CA 95616, USA.
1 constantly, we consider cases with η.
8 pc for the ≥10 14 L ☉ Hot DOGs if they are heavily obscured by graphite-silicate mixed dust grains with a sublimation temperature of.
To compare the far-IR SEDs of hyperluminous quasars and Hot DOGs, we have gathered the available Herschel photometry for our quasar sample. Herschel SPIRE data are available for 15 quasars, and 2 of them also have PACS measurements. This photometry is listed in Table 4.
Figure 2. Mid-IR colors of the hyperluminous ( L bol > 10 14 L ☉ ) Hot DOGs and optically selected hyperluminous quasars. The open squares show the 116 selected quasars; the filled circles show the 20 WISE -selected Hot DOGs. For Hot DOGs not detected in WISE [3.4] and [4.6], their IRAC measurements are plotted with the color correction from IRAC [3.6] to WISE [3.4] and IRAC [4.5] to WISE [4.6] applied.
50 yr in the rest frame. However, the timescale for luminosity changes is more likely to be related to the scale of the dust that produces the peak emission in the SED. In Section 3.2, we show that the highest temperature dust and therefore smallest scale that contributes substantially to the SED is at a temperature of T d.
50 Myr. For a Kerr black hole where η = 0.3 (Thorne 1974), τ Salpeter.
40 pc. Therefore we do not expect large luminosity variations over a rest-frame timescale less than.
Source Redshift L bol L IR L 0.1–1 μ m L 1–20 μ m L > 20 μ m L 5.8 μ m L 7.8 μ m (10 13 L ⊙ ) (10 13 L ⊙ ) (10 13 L ⊙ ) (10 13 L ⊙ ) (10 13 L ⊙ ) (10 13 L ⊙ ) (10 13 L ⊙ ) W0116−0505 3.173 11.7 8.2 0.0 7.8 3.9 0.9 1.0 W0126−0529 2.937 14.7 10.7 0.1 7.0 7.6 1.8 1.3 W0134−2922 3.047 11.3 6.2 0.1 9.0 2.7 1.4 1.2 W0149+2350 3.228 10.4 7.4 0.0 6.2 4.1 0.8 0.8 W0220+0137 3.122 12.9 9.6 0.1 7.6 5.2 1.0 1.1 W0255+3345 2.668 10.4 7.9 0.0 6.8 3.6 0.9 1.1 W0410−0913 3.592 16.8 11.3 0.1 9.3 7.3 1.1 1.0 W0533−3401 2.904 10.4 7.5 0.1 5.7 4.6 0.8 0.8 W0615−5716 3.399 16.5 11.3 0.0 11.0 5.4 1.3 1.4 W0831+0140 3.888 18.0 12.0 0.2 11.0 7.1 1.1 1.1 W0859+4823 3.245 10.0 6.2 0.1 6.6 3.3 0.9 0.8 W1248−2154 3.318 11.8 7.4 0.1 8.0 3.6 1.0 1.0 W1322−0328 3.043 10.1 7.0 0.1 6.6 3.4 0.8 0.9 W1838+3429 3.205 11.1 8.9 0.1 8.6 2.5 0.9 1.4 W2042−3245 3.963 13.7 5.8 0.1 11.4 2.1 1.4 1.1 W2201+0226 2.877 11.9 8.0 0.0 6.6 5.5 1.2 0.9 W2210−3507 2.814 11.7 8.8 0.1 6.3 5.3 1.0 1.0 W2246−0526 4.593 34.9 22.1 0.1 22.2 12.6 1.9 1.8 W2246−7143 3.458 12.1 8.3 0.0 7.8 4.6 1.0 1.0 W2305−0039 3.106 13.9 8.3 0.0 10.1 3.8 1.7 1.4.
0.46 ( z = 2.8). We note that the uncertainties in assumptions on ( z ), M seed , and L ( z ) do not affect the estimate significantly due to the logarithmic scaling (Equation (7)). An order of magnitude uncertainty in these parameters will change the estimate of by 0.1 at the most. T age depends on the when SMBH seeds appear ( z.
The Wide-field Infrared Survey Explorer ( WISE ), which surveyed the entire sky at 3.4, 4.6, 12, and 22 μ m, was designed to identify nearby cool brown dwarfs and the most luminous dusty galaxies in the universe (Wright et al. 2010). By selecting objects with marginal or no detection in the WISE 3.4 and 4.6 μ m bands and strong detections in the 12 and 22 μ m bands, we have discovered a population of hyperluminous galaxies with L bol > 10 13 L ☉ (Eisenhardt et al. 2012; Wu et al. 2012; Bridge et al. 2013). Spectroscopy reveals that these " W 1 W 2-dropouts" are predominantly systems at redshift 1.6 0.3 mJy and F 24 μ m / F R > 1000; Dey et al. 2008), but have hotter dust temperatures (>60 K; Wu et al. 2012; Bridge et al. 2013; Jones et al. 2014) than DOGs (30–40 K; Pope et al. 2008; Melbourne et al. 2012). Thus, we also refer to this population as "Hot DOGs" (Wu et al. 2012).
5. The solid black line shows the mass of a lensing galaxy with size R e.
Note. Redshifts from: V10 (Véron-Cetty & Véron 2010), C04 (Croom et al. 2004), C09 (Croom et al. 2009), S10 (Schneider et al. 2010), P12 (Pâris et al. 2012), DR10 (Ahn et al. 2013), and NED (2013 April version of HyLIRG list from NASA/IPAC Extragalactic Database). Only the first 15 sources are listed here. The complete electronic table of 116 sources is available.
4.4. Spatial Distribution of the Hot Dust.
In 200 years at 10 14 L ☉ , the total energy output is 2.5 × 10 57 erg, or six orders of magnitude higher than the total energy output of a long gamma-ray burst (GRB, E total.
Note. Only photometry of the first 15 sources are listed here. The complete electronic table with photometry of 116 sources is available. The numbers in parentheses are the 1 σ uncertainty in photometry.
The bolometric luminosity L bol is calculated very conservatively by integrating over the photometric data, only considering >3 σ detections, with a power law interpolated between observed flux density measurements, and extrapolated to 20% beyond the shortest and longest wavelength bands by assuming no luminosity beyond these wavelengths. We do not incorporate any extinction correction or SED model in our luminosity estimate. The resulting luminosity values from this approach can be considered as conservative lower limits. If the best-fit SED templates or spline-smoothed SEDs are considered, the luminosity values typically increase by a factor of 2.
8 × 10 13 L ☉ , slightly shy of our L bol threshold, but likely making it one of the most powerful starburst systems known. In addition to Herschel studies, a few systems discovered by WISE using different selection criteria have L bol at the.
22.4 mag corresponds to a lensing mass of 2 × 10 9 M ☉ , and an Einstein radius of.
The luminosities reported in this paper are calculated based on the assumption of isotropic emission in the observed wavebands. If the escaped energy is beamed, the intrinsic luminosity could be significantly overestimated. However, beaming, which is observed in blazars, is associated with variable light curves. In addition, Hot DOGs are only weakly detected or undetected in shallow (1 mJy), wide-area radio surveys (C.-W. Tsai et al. 2015, in preparation), unlike beamed objects which are typically radio bright (Urry & Padovani 1995).
Abstract.
2–3 mag redder in [4.6]–[12] color. The Hot DOG redshifts span 2.8.
10 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA.
3.1. Color–Color Diagram.
2 × 10 10 M ☉ is needed, with higher masses for a Salpeter (1955) IMF. These must be formed within a few Myr—the lifetime of massive stars which produce most of the Lyman continuum photons. The implied star formation rate is SFR > 5 × 10 3 M ☉ yr −1 , at least an order of magnitude higher than known extreme starburst systems such as sub-millimeter galaxies (Michałowski et al. 2010; Swinbank et al. 2014) or Lyman break galaxies (Shapley et al. 2005) at high redshift. Large masses of molecular gas and cold dust should accompany this level of star formation, but we observe neither substantial CO emission from these systems (A. Blain et al. 2015, in preparation) nor abundant cold dust (Wu et al. 2012; Jones et al. 2014). Thus we conclude, as did Eisenhardt et al. (2012), that a starburst is unlikely to be the dominant mechanism driving the high luminosity in Hot DOGs.
40 μ m, well beyond the WISE 22 μ m ( W 4) filter. To identify such sources would require deeper imaging at 30–70 μ m from future missions such as SPICA , or submillimeter photometry at 200 μ m—1 mm with ALMA or CCAT. As noted by Assef et al. (2015), such objects may also have been detected by WISE but failed to meet the W 1 W 2-dropout selection, because they will be detectable by WISE at 3.4 and 4.6 μ m. If we relax the W 1 and W 2 flux limits for Hot DOGs, many contaminants fall into the selection criteria, making it much more difficult to identify the ELIRG systems. It is also possible that AGNs at.
Figure 10 shows L bol versus z for hyperluminous Hot DOGs and quasars, and for quasars at z > 6. The curves in the Figure show the luminosity versus redshift tracks followed by black holes as they grow for various choices of M seed and η . Although in reality the Eddington ratio is likely to vary, the overall averaged Eddington ratio should be lower than unity. With the assumption of.
We have obtained high angular resolution (PSF FWHM 0 15) near-IR imaging of over 30 Hot DOGs, including 5 ELIRGs reported in this paper, with the NIRC2 camera on Keck-II with adaptive optics, and with HST . These images do not show lensing features such as multiple images or arcs (Wu et al. 2014; S. Petty et al. 2015, in preparation; C. R. Bridge et al. 2015, in preparation). For the six ELIRGs in our sample with high-resolution near-IR imaging data, it is not uncommon to see other objects a few arcseconds from the ELIRGs in the images from HST or Keck with adaptive optics. However, these objects' morphologies are typical of recent or ongoing mergers, rather than characteristic lensing geometries, based on our experience with strong lensing work (Eisenhardt et al. 1996; Moustakas et al. 2007). There are sources which fall in the gray shaded area in Figure 6, but in no case is the θ E corresponding to the inferred mass as large as their separation from the ELIRG. Thus, unless the lensing galaxies are anomalously faint or highly obscured, the high luminosity of Hot DOGs seems to be intrinsic rather than due to gravitational lensing.
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192 Myr. In other words, a non-spinning black hole experiences less radiation feedback to accreting material due to its lower radiation efficiency, thus its mass doubling time could be 3 times shorter than a fast spinning black hole.
0.3 for a rapidly spinning black hole. The radiative efficiency is a factor of 3 higher for a Kerr black hole because the material can still radiate gravitational energy to the last stable circular orbit, which is three times smaller compared to a non-spinning Schwarzschild black hole or a slowly spinning black hole (Thorne 1974). The curves on Figure 10 represent the theoretical limits of black hole mass growth, and the objects toward the upper right of the curves can not be produced with the given initial seed mass and radiative efficiency unless the SMBH is in a super-Eddington state for a significant period of its history.
Assuming black holes of seed mass M seed appear at z.
100 Myr, likely to be the upper bound for Hot DOG phase. This timescale is a few times the Salpeter timescale. The accreted mass onto the SMBH exceeds 7 × 10 9 M ☉ .
Figure 5. Photometry and angular separation of WISE W 1 sources within 100'' of the ELIRGs. Data points are color-coded by indiv >
Case 1 is addressed by Figure 5, which shows the W 1 photometry versus separation for objects in the 20 ELIRG fields. We use a SWIRE elliptical galaxy SED template and assume a total mass-to-light ratio of M / L B.
60 K (Wu et al. 2012; Bridge et al. 2013). Ground-based sub-millimeter follow-up observations of Hot DOGs indicate the rest-frame far-IR luminosity of Hot DOGs is about an order of magnitude lower than the rest-frame mid-IR luminosity (Wu et al. 2012; Jones et al. 2014). Considering the three SED components introduced in Section 3.3, the blue component (0.1–1 μ m) represents direct emission from the host galaxy, as well as direct or scattered emission from the AGN and its accretion disk; the mid-IR component (1–20 μ m) represents emission from the AGN dust torus, or dust emission from the cocoon of highly obscured AGNs; and the >20 μ m component represents far-IR emission from dust at the outskirts of the AGN, or starburst-powered dust emission from the host galaxy.
a Redshift from Wu et al. (2012).
Source R -band 3.4 μ m 4.6 μ m 12 μ m 22 μ m 70 μ m 160 μ m 250 μ m 350 μ m 500 μ m (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) J000322.910−260316.80 0.40(0.11) 0.86(0.02) 0.69(0.02) 2.2(0.1) 8.5(0.9) ⋯ ⋯ ⋯ ⋯ ⋯ J001527.400+064012.00 0.43(0.12) 0.93(0.02) 1.09(0.03) 5.3(0.2) 10.9(1.1) ⋯ ⋯ ⋯ ⋯ ⋯ J004131.500−493612.00 0.79(0.22) 1.61(0.04) 1.62(0.04) 4.3(0.1) 9.1(0.8) ⋯ ⋯ ⋯ ⋯ ⋯ J010311.300+131618.00 1.09(0.30) 1.08(0.03) 1.51(0.04) 9.0(0.2) 19.4(1.0) ⋯ ⋯ ⋯ ⋯ ⋯ J012156.038+144823.94 0.31(0.09) 0.93(0.03) 1.16(0.03) 3.6(0.2) 9.2(1.0) ⋯ ⋯ ⋯ ⋯ ⋯ J012412.470−010049.76 0.45(0.12) 1.28(0.03) 1.40(0.03) 3.6(0.1) 6.7(1.0) ⋯ ⋯ ⋯ ⋯ ⋯ J013301.900−400628.00 0.49(0.13) 0.65(0.02) 0.89(0.03) 3.4(0.1) 9.4(0.9) ⋯ ⋯ ⋯ ⋯ ⋯ J015636.000+044528.00 0.43(0.12) 0.60(0.02) 0.67(0.02) 2.2(0.1) 3.1(0.8) ⋯ ⋯ ⋯ ⋯ ⋯ J020727. 200−374156.00 0.85(0.23) 1.49(0.03) 1.71(0.04) 6.0(0.1) 12.3(0.8) ⋯ ⋯ ⋯ ⋯ ⋯ J020950.712−000506.49 0.63(0.17) 0.93(0.02) 1.36(0.03) 6.1(0.2) 15.0(0.8) ⋯ ⋯ 66(6) 48(6) 22(7) J024008.100−230915.00 1.01(0.28) 1.92(0.04) 3.23(0.07) 11.1(0.2) 21.1(1.0) ⋯ ⋯ ⋯ ⋯ ⋯ J024854.300+180250.00 0.17(0.05) 0.62(0.02) 0.55(0.02) 1.6(0.1) 4.1(1.1) ⋯ ⋯ ⋯ ⋯ ⋯ J025240.100−553832.00 0.88(0.24) 1.73(0.04) 1.99(0.04) 8.2(0.2) 19.0(0.9) ⋯ ⋯ 46(2) 39(3) 14(3) J030722.800−494548.00 0.06(0.02) 0.54(0.01) 0.51(0.02) 1.1(0.1) 4.0(0.7) ⋯ ⋯ ⋯ ⋯ ⋯ J032108.450+413220.87 0.56(0.15) 1.39(0.03) 1.94(0.05) 6.8(0.2) 12.7(1.1) ⋯ ⋯ ⋯ ⋯ ⋯
4.5. Energy Source Other than AGNs?
200 yr, or many centuries in the observed frame. As noted in Section 4.1, the flux variation at 12 and 22 μ m is less than 30% over a six-month period based on WISE observations.
2 Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095-1547, USA.
1300 sources with estimated L bol > 5 × 10 13 L ☉ in the optical, near-IR, and m >14 L ☉ , assuming their emission is isotropic.
10 14 L ☉ level (Lonsdale et al. 2015; D. Stern et al. 2015, in preparation), but they all show obvious AGN features in their spectra or have radio emission.
Analysis of the black hole mass function at z = 0 suggests that SMBHs spend.
In Figure 10, a few quasars at z > 6 have implied black hole mass 10 9 M ☉ at an age of 10 15 L ☉ by z.
For the ELIRG Hot DOGs at 2.8 z 4.6, we assume the current value ( z )
2.2. Far-IR and Submillimeter Observations.
Table 5. Luminosities of WISE ELIRGs.
On the other hand, Assef et al. (2015) have studied the luminosity functions of Hot DOGs and luminous quasars, finding they have comparable number density. This suggests similar lifetimes for both the obscured and the unobscured phases of hyperluminous black hole accretion. Using the life cycle of broad line quasars at z = 1 (Kelly et al. 2010) as an analog, this time scale is.
0 25 position uncertainty of W1248–2154 in AllWISE images. The black dashed circle indicates an r = 1'' region. The object on the right of the red cross is at z = 3.326, and the source on the left lies just outs circle is at z = 0.339.
0.2–0.3 is adopted, the higher radiative efficiency means that the SMBH accumulates less mass to produce the same luminosity. Assuming black hole merging is not important, black holes with η = 0.3 cannot produce the observed ELIRGs and z > 6 quasars unless their seed mass M seed 10 4 M ☉ or/and they have been accreting at super-Eddington rates since their formation in the early universe. For the most luminous Hot DOGs and quasars, the required seed mass is M seed > 10 7 M ☉ , higher than the most massive seed masses predicted by current models (Begelman et al. 2008; Agarwal et al. 2012; Hosokawa et al. 2013). On the other hand, for η = 0.1 (dotted lines in Figure 10), relatively modest seed black holes can grow to Hot DOGs if they are accreting at ( z ) > 0.4. If the seed mass exceeds 10 4 M ☉ , even accretion rates 6 and ELIRGs at z 3.5 implies a constraint on the upper limit to the radiative efficiency for given seed black hole mass values. In Figure 11, we show the upper limits of radiative efficiency in the cases of M seed = 10 3 M ☉ and M seed = 10 6 M ☉ . The first case represents the upper bound on the predicted black hole seed mass from the first stars (Hirano et al. 2014 and references therein). The 10 6 M ☉ case is upper bound of the seed mass from direct collapse of pristine gas clouds (Agarwal et al. 2012), or from rapid mass accretion onto primordial massive stars (Hosokawa et al. 2013). The hyperluminous Hot DOGs and quasars at z > 3.5 place similar constraints on black hole radiative efficiency η as z > 6 quasars. If the black hole seeds have masses of.
Footnotes.
Beaming implies small physical scales, hence the potential for rapid variability. We do not see significant variation in the WISE data. None of the Hot DOGs varies in W 3 and W 4 to a limit of 30% over 6 months, and none are flagged as significantly varying in the AllWISE catalog. Finally, many Hot DOGs have emission-line spectra (Wu et al. 2012; P. R. M. Eisenhardt et al. 2015, in preparation), unlike the featureless spectral characteristic of BL Lac objects. These properties distinguish Hot DOGs from known beamed populations.
The high luminosities in the ELIRG Hot DOGs are likely maintained by M BH.
9 Astronomy Department, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa.
Table 2. Photometry of WISE ELIRGs.
2 × 10 10 M ☉ (McConnell et al. 2011) would have over the Hubble time.
Although super-Eddington accretion (i.e., ( z ) > 1) is considered to be an unstable phase, it has been suggested to be common at z > 1.7 (Steinhardt & Elvis 2010). It is possible that Hot DOGs are in a transitional super-Eddington phase which produces their extraordinary luminosity. Indeed, super-Eddington accretion is commonly invoked to explain the non-nuclear "ultraluminous X-ray" source populations seen in local galaxies (e.g., Bachetti et al. 2014). However, super-Eddington accretion requires a special configuration for the accretion disk, and the timescales for super Eddington accretion in AGNs are not thoroughly investigated and understood. Begelman (2002) suggests that the Eddington limit can be exceeded by 10–100 times via small scale inhomogeneities in the thin disk accretion. Ohsuga & Mineshige (2007) suggest accreting material through the photon trapping regions around the accreting black hole can help the system stably bypass the radiation feedback. Statistical study of SDSS quasars suggests the maximum Eddington ratio for Type 1 quasars is.
Table 4. Photometry of Optically Selected Quasars with L bol > 10 14 L ☉ (Short Version)
40 times the mass annually accreted by the SMBH in Hot DOGs. This timescale is shorter than the light-crossing timescale of 200 yr discussed in Section 4.4.
3 (Figure 9). Hence we suggest that ν L ν at 5.8 or 7.8 μ m as an estimate of total bolometric AGN luminosity should be used with caution.
The raw images were dark-subtracted and then sky-subtracted using a sky frame based on the median average of all frames, and a dome flat 19 was used to correct for pixel-to-pixel sensitivity variations. The co-added image (Figure 7) is the median average of aligned single frame images based on the pixel location of a star in the field. The FWHM of point-like sources in the field is.
Here we examine the most luminous Hot DOGs identified, corresponding to galaxies with L bol > 10 14 L ☉ . Luminosities this high correspond to a star formation rate of many thousands of solar masses per year, or to an SMBH accretion rate of tens of solar masses per year. If this luminosity is maintained for.
Received 2014 October 6 Accepted 2015 March 4 Published 2015 May 22.
First, we consider what may be inferred from the WISE imaging data, estimating upper bounds on the possible magnification. Significant lensing requires the magnified source to be close to the effective Einstein radius ( θ E ) of the lens. In general, θ E is governed by the redshifts of background target and foreground lens, as well as the mass of the lens. In Case 1, θ E is larger than the angular resolution of W 1 (6''). In Case 2, θ E is smaller than 6'' and the lensed images and foreground lens could be blended.
3.2. SEDs.
4.1. Possible Effects of Beaming?
We use the STARBURST99 simulation (Leitherer et al. 2010) with instantaneous starburst models to estimate the star formation needed to produce such a Lyman continuum photon rate. For a flat IMF (observed in compact starbursts in extreme environments such as young and massive clusters near the Galactic center—Figer et al. 1999, 2002), a total star formation of.
20 is plotted on the top. The black hole mass for an Eddington ratio of one ( ) is plotted on the right. The dotted, dashed, and sol > and radiative efficiency η = 0.1, 0.2, and 0.3, respectively. The magenta lines show predictions with initial black hole mass M seed = 10 3 M ☉ , while yellow lines show the case of M seed = 10 6 M ☉ . The regions to the top and right of each curve require significant periods of super-Eddington accretion for the curve's seed mass and radiative efficiency. The red dots show ELIRG Hot DOGs, the blue dots show ELIRG quasars, and the green dots show resulting quasars at z > 6 based on Blain et al. (2013, and references therein).
1.2 × 10 10 M ☉ (Wu et al. 2015). Using our methodology, the luminosity of this source is 1.6 × 10 14 L ☉ .
Based on the Hot DOG SEDs, we suggest that emission from a dust component at T d.
4.7. High Luminosity State Timescale.
Galaxies with masses >10 13 M ☉ exist, such as ESO 146-5 ( 10 13 M ☉ ; Carrasco et al. 2010), which dominates the Abell 3827 cluster of galaxies, but massive galaxy clusters are not in evidence near the ELIRGs (Griffith et al. 2012; Assef et al. 2015). We conclude that the resolved individual WISE sources that we detect are not likely to be able to cause strong magnification of the ELIRGs.
10 14.5 L ☉ have reached a physical limit for BH accretion, or that the accreting material is depleted after z.
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