We present Keck-Adaptive Optics and Hubble Space Telescope high resolution near-infrared (IR) imaging for 500 µm-bright candidate lensing systems identified by the Herschel Multi-tiered Extragalactic Survey (HerMES) and Herschel Astrophysical Terahertz Survey (H-ATLAS). Out of 87 candidates with near-IR imaging, 15 (∼ 17%) display clear near-IR lensing morphologies. We present near-IR lens models to reconstruct and recover basic rest-frame optical morphological properties of the background galaxies from 12 new systems. Sources with the largest near-IR magnification factors also tend to be the most compact, consistent with the size bias predicted from simulations and previous lensing models for sub-millimeter galaxies. For four new sources that also have high-resolution sub-mm maps, we test for differential lensing between the stellar and dust components and find that the 880 µm magnification factor (µ 880 ) is ∼ 1.5 times higher than the near-IR magnification factor (µ NIR ), on average. We also find that the stellar emission is ∼ 2 times more extended in size than dust. The rest-frame optical properties of our sample of Herschel-selected lensed SMGs are consistent with those of unlensed SMGs, which suggests that the two populations are similar. c AB mag 1HerMES S250 J002854.0-420457 HELAISS04 J = 62 × 4 J = 25.8 1HerMES S250 J002906.3-421420 HELAISS01 J = 62 × 4 J = 25.4 1HerMES S250 J003823.7-433705 HELAISS02 J = 125 × 4 J = 25.7 1HerMES S250 J021620.0-032520 HXMM26 Kp = 60 × 30 Kp = 25.6 e 1HerMES S250 J021632.1-053422 HXMM14 J = 125 × 4 J = 25.6 1HerMES S250 J021830.6-053125 HXMM02 J = 177 × 4, Kp = 60 × 18 J = 26.3, Kp = 25.6 e 1HerMES S250 J021836.7-035316 HXMM13 J = 62 × 4 J = 25.6 1HerMES S250 J021942.9-052433 HXMM20 J = 125 × 4 J = 25.6 1HerMES S250 J022016.6-060144 HXMM01 J = 62 × 4, Ks = 80 × 35 J = 25.5, Ks = 25.6 1HerMES S250 J022021.8-015329 HXMM04 J = 62 × 4 J = 25.6 1HerMES S250 J022029.2-064846 HXMM09 J = 62 × 4, H = 120 × 12, K = 80 × 15 J = 25.2, H = 24.8, K = 24.5 1HerMES S250 J022135.2-062618 HXMM03 J = 62 × 4 J = 25.4 1HerMES S250 J022201.7-033340 HXMM11 Ks = 100 × 18 Ks = 25.6 e 1HerMES S250 J022205.5-070727 HXMM23 J = 62 × 4 J = 25.2 1HerMES S250 J022212.9-070224 HXMM28 J = 125 × 4 J = 25.6 1HerMES S250 J022250.8-032414 HXMM22 J = 62 × 4 J = 25.4 1HerMES S250 J022515.3-024707 HXMM19 J = 62 × 4 J = 25.3 1HerMES S250 J022517.5-044610 HXMM27 J = 62 × 4 J = 25.6 1HerMES S250 J022547.9-041750 HXMM05 J = 62 × 4 J = 25.8 1HerMES S250 J023006.0-034153 HXMM12 J = 62 × 4 J = 25.2 1HerMES S250 J032434.4-292646 HECDFS08 J = 62 × 4 J = 25.4 1HerMES S250 J032443.1-282134 HECDFS03 J = 125 × 4 J = 25.4 1HerMES S250 J032636.4-270045 HECDFS05 J = 62 × 4 J = 25.6 1HerMES S250 J032712.7-285106 HECDFS09 J = 62 × 4 J = 25.5 1HerMES S250 J033118.0-272015 HECDFS11 J = 62 × 4 J = 25.3 1HerMES S250 J033210.8-270536 HECDFS04 J = 62 × 4 J = 26.0 1HerMES S250 J033732.5-295353 HECDFS02 J = 177 × 4 J = 26.8 1HerMES S250 J043340.5-540338 HADFS04 J = 62 × 4 J = 25.6 1HerMES S250 J043829.8-541832 HADFS02 J = 62 × 4 J = 25....
We present Hubble Space Telescope (HST) WFC3 imaging and grism spectroscopy observations of the Herschel-selected gravitationally-lensed starburst galaxy HATLASJ1429-0028. The lensing system consists of an edge-on foreground disk galaxy at z = 0.218 with a nearly complete Einstein ring of the infrared luminous galaxy at z = 1.027. The WFC3 spectroscopy with G102 and G141 grisms, covering the wavelength range of 0.8 to 1.7 µm, resulted in detections of Hα+[NII], Hβ, [SII], and [OIII] for the background galaxy from which we measure line fluxes and ratios. The Balmer line ratio Hα/Hβ of 7.5 ± 4.4, when corrected for [NII], results in an extinction for the starburst galaxy of E(B − V ) = 0.8 ± 0.5. The Hα based star-formation rate, when corrected for extinction, is 60 ± 50 M ⊙ yr −1 , lower than the instantaneous star-formation rate of 390 ± 90 M ⊙ yr −1 from the total IR luminosity. We also compare the nebular line ratios of HATLASJ1429-0028 with other star-forming and sub-mm bright galaxies. The nebular line ratios are consistent with an intrinsic ultra-luminous infrared galaxy with no evidence for excitation by an active galactic nucleus (AGN). We estimate the metallicity, 12 + log(O/H), of HATLASJ1429-0028 to be 8.49 ± 0.16. Such a low value is below the average relations for stellar mass vs. metallicity of galaxies at z ∼ 1 for a galaxy with stellar mass of ∼ 2 × 10 11 M ⊙ . The combination of high stellar mass, lack of AGN indicators, low metallicity, and the high star-formation rate of HATLASJ1429-0028 suggest that this galaxy is currently undergoing a rapid formation.
We present the results of combined deep Keck/NIRC2, HST/WFC3 near-infrared and Herschel far infrared observations of an extremely star forming dusty lensed galaxy identified from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS J133542.9+300401). The galaxy is gravitationally lensed by a massive WISE identified galaxy cluster at z ∼ 1. The lensed galaxy is spectroscopically confirmed at z = 2.685 from detection of CO(1 → 0) by GBT and from detection of CO(3 → 2) obtained with CARMA. We use the combined spectroscopic and imaging observations to construct a detailed model of the background dusty lensed sub-millemter galaxy (SMG) which allows us to study the source plane properties of the target. The best-fit lens model provide magnification of µ star = 2.10±0.11 and µ dust = 2.02±0.06 for the stellar and dust components respectively. Multi-band data yields a magnification corrected star formation rate of 1900(±200) M yr −1 and stellar mass of 6.8 +0.9 −2.7 × 10 11 M consistent with a main sequence of star formation at z ∼ 2.6. The CO observations yield a molecular gas mass of 8.3(±1.0) × 10 10 M , similar to the most massive star-forming galaxies, which together with the high star-formation efficiency are responsible for the intense observed star formation rates. The lensed SMG has a very short gas depletion time scale of ∼ 40 Myr. The high stellar mass and small gas fractions observed indicate that the lensed SMG likely has already formed most of its stellar mass and could be a progenitor of the most massive elliptical galaxies found in the local Universe.
We present the rest-frame optical spectral energy distribution (SED) and stellar masses of six Herschel-selected gravitationally lensed dusty, star-forming galaxies (DSFGs) at 1 < z < 3. These galaxies were first identified with Herschel/SPIRE imaging data from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) and the Herschel Multi-tiered Extragalactic Survey (HerMES). The targets were observed with Spitzer/IRAC at 3.6 and 4.5 μm. Due to the spatial resolution of the IRAC observations at the level of 2″, the lensing features of a background DSFG in the near-infrared are blended with the flux from the foreground lensing galaxy in the IRAC imaging data. We make use of higher resolution Hubble/WFC3 or Keck/NIRC2 Adaptive Optics imaging data to fit light profiles of the foreground lensing galaxy (or galaxies) as a way to model the foreground components, in order to successfully disentangle the foreground lens and background source flux densities in the IRAC images. The flux density measurements at 3.6 and 4.5 μm, once combined with Hubble/WFC3 and Keck/NIRC2 data, provide important constraints on the rest-frame optical SED of the Herschel-selected lensed DSFGs. We model the combined UV-to millimeter-wavelength SEDs to establish the stellar mass, dust mass, star formation rate, visual extinction, and other parameters for each of these Herschel-selected DSFGs. These systems have inferred stellar masses in the range 8 × 10 10-4 × 10 11 M e and star formation rates of around 100 M e yr −1. This puts these lensed submillimeter systems well above the SFR-M * relation observed for normal star-forming galaxies at similar redshifts. The high values of SFR inferred for these systems are consistent with a major merger-driven scenario for star formation.
We present a source-plane reconstruction of a Herschel and Planck-detected gravitationally lensed dusty starforming galaxy (DSFG) at z=1.68 using Hubble, Submillimeter Array (SMA), and Keck observations. The background submillimeter galaxy (SMG) is strongly lensed by a foreground galaxy cluster at z=0.997 and appears as an arc with alength of ∼15″ in the optical images. The continuum dust emission, as seen by SMA, is limited to a single knot within this arc. We present a lens model with source-plane reconstructions at several wavelengths to show the difference in magnification between the stars and dust, and highlight the importance ofmulti-wavelength lens models for studies involving lensed DSFGs. We estimate the physical properties of the galaxy by fitting the flux densities to model spectral energy distributions leading to a magnification-corrected starformation rate (SFR) of 390±60 M yr −1 and a stellar mass of 1.1 0.4 10 11 M . These values are consistent with high-redshift massive galaxies that have formed most of their stars already. The estimated gas-to-baryon fraction, molecular gas surface density, and SFR surface density have values of 0.43±0.13, 350±200 M pc −2 , and~ 12 7 M yr −1 kpc −2 , respectively. The ratio of SFR surface density to molecular gas surface density puts this among the most star-forming systems, similar to other measured SMGs and local ULIRGs.
We measure the cosmic microwave background (CMB) skewness power spectrum in Planck, using frequency maps of the HFI instrument and the Sunyaev-Zel'dovich (SZ) component map. The two-to-one skewness power spectrum measures the cross-correlation between CMB lensing and the thermal SZ effect. We also directly measure the same cross-correlation using the Planck CMB lensing map and the SZ map and compare it to the crosscorrelation derived from the skewness power spectrum. We model fit the SZ power spectrum and CMB lensing-SZ cross-power spectrum via the skewness power spectrum to constrain the gas pressure profile of dark matter halos. The gas pressure profile is compared to existing measurements in the literature including a direct estimate based on the stacking of SZ clusters in Planck.
Follow-up observations of (sub-)mm-selected gravitationally lensed systems have allowed a more detailed study of the dust-enshrouded phase of star formation up to very early cosmic times. Here, the case of the gravitationally lensed merger in HATLAS J142935.3–002836 (also known as H1429−0028; zlens = 0.218, zbkg = 1.027) is revisited following recent developments in the literature and new Atacama Pathfinder EXperiment (APEX) observations targeting two carbon monoxide (CO) rotational transitions Jup = 3 and 6. We show that the line profiles comprise three distinct velocity components, where the fainter high velocity one is less magnified and more compact. The modelling of the observed spectral line energy distribution of CO Jup = 2–6 and [C i] 3P1−3P0 assumes a large velocity gradient scenario, where the analysis is based on four statistical approaches. Since the detected gas and dust emission comes exclusively from only one of the two merging components (the one oriented north–south, NS), we are only able to determine upper limits for the companion. The molecular gas in the NS component in H1429−0028 is found to have a temperature of ∼70 K, a volume density of log (n[cm−3]) ∼ 3.7, to be expanding at ∼10 km s−1 pc−1, and amounts to ${M_{\rm H_2} = 4_{-2}^{+3} \times 10^9\,{\rm M}_\odot }$. The CO to H2 conversion factor is estimated to be $\alpha _{\rm CO} = 0.4_{-0.2}^{+0.3}\,$ M⊙/(K km s−1 pc2). The NS galaxy is expected to have a factor of ≳10× more gas than its companion (${M_{\rm H_2}}\lesssim 3\times 10^8$ M⊙). Nevertheless, the total amount of molecular gas in the system comprises only up to 15 per cent (1σ upper limit) of the total (dynamical) mass.
Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present the detection at 89 μm (observed frame) of the Herschel-selected gravitationally lensed starburst galaxy HATLAS J1429-0028 (also known as G15v2.19) in 15 minutes with the High-resolution Airborne Wideband Camera-plus (HAWC+) onboard the Stratospheric Observatory for Infrared Astronomy (SOFIA). The spectacular lensing system consists of an edge-on foreground disk galaxy at z=0.22 and a nearly complete Einstein ring of an intrinsic ultra-luminous infrared (IR) galaxy at z=1.03. Is this high IR luminosity powered by pure star formation (SF) or also an active galactic nucleus (AGN)? Previous nebular line diagnostics indicate that it is star formation dominated. We perform a 27-band multiwavelength spectral energy distribution (SED) modeling including the new SOFIA/HAWC+ data to constrain the fractional AGN contribution to the total IR luminosity. The AGN fraction in the IR turns out to be negligible. In addition, J1429-0028 serves as a testbed for comparing SED results from different models/templates and SED codes (MAGPHYS, SED3FIT, and CIGALE). We stress that star formation history is the dominant source of uncertainty in the derived stellar mass (as high as a factor of ∼10) even in the case of extensive photometric coverage. Furthermore, the detection of a source at z∼1 with SOFIA/HAWC+ demonstrates the potential of utilizing this facility for distant galaxy studies including the decomposition of SF/ AGN components, which cannot be accomplished with other current facilities.
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