KINGFISH—Key Insights on Nearby Galaxies: A Far-Infrared Survey with<i>Herschel</i>: Survey Description and Image Atlas1

Kennicutt, Robert C.; Calzetti, Daniela; Aniano, G.; Appleton, P. N.; Armus, L.; Beirão, P.; Bolatto, Alberto D.; Brandl, Bernhard R.; Crocker, Alison F.; Croxall, K. V.; Dale, Daniel A.; Meyer, Jackie-Ruth; Draine, B. T.; Engelbracht, C. W.; Galametz, M.; Gordon, K. D.; Groves, Brent; Hao, Cai-Na; Hélou, G.; Hinz, J. L.; Hunt, L. K.; Johnson, Benjamin D.; Koda, Jin; Krause, O.; Leroy, Adam K.; Li, Y.; Meidt, Sharon E.; Montiel, Edward; Murphy, E. J.; Rahman, Nurur; Rix, H. W.; Roussel, H.; Sandström, Karin; Sauvage, M.; Schinnerer, E.; Skibba, Ramin; Smith, John David; Srinivasan, S.; Vigroux, L.; Walter, Fabian; Wilson, C. D.; Wolfire, M. G.; Zibetti, S.

doi:10.1086/663818

Cited by 389 publications

(308 citation statements)

References 154 publications

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“…For galaxies that were observed as part of the KINGFISH (Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel; Kennicutt et al 2011) program, IC 342 and NGC 6946, we use the PACS images made with the Scanamorphos code version 16.9. The FWHM angular resolutions are approximately 6 0, 5 8, 7 8, and 12″ at 24 μm, 70 μm, 100 μm, and 160 μm, respectively.…”

Section: Infrared Datamentioning

confidence: 99%

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

Tan

Gao

Zhang

et al. 2018

ApJ

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We present J HCN 4 3 =  and J HCO 4 3 =  + maps of six nearby star-forming galaxies, NGC 253, NGC 1068, IC 342, M82, M83, and NGC 6946, obtained with the James Clerk Maxwell Telescope as part of the MALATANG survey. All galaxies were mapped in the central 2′×2′region at 14″ (FWHM) resolution (corresponding to linear scales of ∼0.2-1.0 kpc). The L IR -L′ dense relation, where the dense gas is traced by the J HCN 4 3 =  and the J HCO 4 3 =  + emission, measured in our sample of spatially resolved galaxies is found to follow the linear correlation established globally in galaxies within the scatter. We find that the luminosity ratio, L IR /L′ dense , shows systematic variations with L IR within individual spatially resolved galaxies, whereas the galaxy-integrated ratios vary little. A rising trend is also found between L IR /L′ dense ratio and the warm-dust temperature gauged by the 70 μm/100 μm flux ratio. We find that the luminosity ratios of IR/HCN (4-3) and IR/HCO + (4-3), which can be taken as a proxy for the star formation efficiency (SFE) in the dense molecular gas

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Section: Infrared Datamentioning

confidence: 99%

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

Tan

Gao

Zhang

et al. 2018

ApJ

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“…The SFRS sample comprises nuclear and extranuclear starforming regions in 56 nearby galaxies (d < 30 Mpc) observed as part of the SINGS (Kennicutt et al 2003) and KINGFISH (Kennicutt et al 2011) legacy programs. Each of these nuclear and extranuclear star-forming complexes have mid-infrared [i.e., low resolution from 5 to 14 μm (0 3 × 0 9) and high resolution from 10 to 37 μm (0 3 × 0 4)] spectral mappings carried out by the IRS instrument on board Spitzer, and 47″×47″ Herschel/PACS far-infrared spectral mappings for a combination of the principal atomic ISM cooling lines of [O I] NGC 5194 and NGC 2403 are exceptions; these galaxies were part of the SINGS sample, but are not formally included in KINGFISH.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Building on that work, we obtained 33 GHz imaging for the SFRS using the VLA, allowing us to map the 33 GHz emission from each region on 2″ scales, compared to the ≈25″ single-beam GBT photometry. These galaxies, which are included in the Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al 2003) and Key Insights on Nearby Galaxies: a FarInfrared Survey with Herschel (KINGFISH; Kennicutt et al 2011) legacy programs, are well studied and have a wealth of ancillary data available. We are currently in the process of reducing and imaging complementary interferometric observations at matched resolution in the S-(2-4 GHz) and bands (VLA/13B-215; PI.…”

Section: Introductionmentioning

confidence: 99%

The Star Formation in Radio Survey: Jansky Very Large Array 33 GHz Observations of Nearby Galaxy Nuclei and Extranuclear Star-forming Regions

Murphy

Dong

Momjian

et al. 2018

ApJS

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We present 33 GHz imaging for 112pointings toward galaxy nuclei and extranuclear star-forming regions at ≈2″ resolution using the KarlG.Jansky VeryLargeArray (VLA) as part of the Star Formation in Radio Survey. A comparison with 33 GHz Robert C.ByrdGreenBankTelescope single-dish observations indicates that the interferometric VLA observations recover 78%±4% of the total flux density over 25″ regions(≈kpc scales) among all fields. On these scales, the emission being resolved out is most likely diffuse non-thermal synchrotron emission. Consequently, on the ≈30-300 pc scales sampled by our VLA observations, the bulk of the 33 GHz emission is recovered and primarily powered by free-free emission from discrete H II regions, making it an excellent tracer of massive star formation. Of the 225 discrete regions used for aperture photometry, 162 are extranuclear (i.e., having galactocentric radii r G 250 pc) and detected at >3σ significance at 33 GHz and in Hα. Assuming a typical 33 GHz thermal fraction of 90%, the ratio of optically-thin 33 GHz to uncorrected Hα star formation rates indicates a median extinction value on ≈30-300 pc scales of A Hα ≈1.26±0.09 mag, with an associated median absolute deviation of 0.87 mag. We find that 10% of these sources are "highly embedded" (i.e., A Hα 3.3 mag), suggesting that on average, H II regions remain embedded for 1 Myr. Finally, we find the median 33 GHz continuum-to-Hα line flux ratio to be statistically larger within r G <250 pc relative to the outer disk regions by a factor of 1.82±0.39, while the ratio of 33 GHz to 24 μm flux densities is lower by a factor of 0.45±0.08, which may suggest increased extinction in the central regions.

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“…The targeted galaxies cover a wide range of star formation rate (0.02-11 M ☉ yr −1 ), infrared-to-optical luminosity ratio (0.02-6.2), and total gas mass (10 7.8 -10 10.3 M ☉ ). For more information on the target selection, including the mapped regions within sample galaxies, see Kennicutt et al (2011).…”

Section: Pacs Observationsmentioning

confidence: 99%

“…KINGFISH (Key Insights on Nearby Galaxies-a Far-Infrared Survey with Herschel; Kennicutt et al 2011) has investigated a diverse sample of galaxies in the nearby universe (d30 Mpc). Here we explore resolved maps of [C II] across the KINGFISH sample in order to delineate the principal physical drivers of the deficit itself.…”

Section: Introductionmentioning

confidence: 99%

The Spatially Resolved Cooling Line Deficit in Galaxies

Smith

Croxall

Draine

et al. 2016

ApJ

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We present [C II] 158 μm measurements from over 15,000 resolved regions within 54 nearby galaxies of the KINGFISH program to investigate the so-called [C II] "line-cooling deficit" long known to occur in galaxies with different luminosities. The [C II]/TIR ratio ranges from above 1% to below 0.1% in the sample, with a mean value of 0.48±0.21%. We find that the surface density of 24 μm emission dominates this trend, with [C II]/TIR dropping as n m n I 24 m ( )increases. Deviations from this overall decline are correlated with changes in the gas-phase metal abundance, with higher metallicity associated with deeper deficits at a fixed surface brightness. We supplement the local sample with resolved [C II] measurements from nearby luminous infrared galaxies and highredshift sources from z=1.8-6.4, and find that star formation rate density drives a continuous trend of deepening [C II] deficit across six orders of magnitude in S SFR . The tightness of this correlation suggests that an approximate S SFR can be estimated directly from global measurements of [C II]/TIR, and a relation is provided to do so. Several low-luminosity active galactic nucleus (AGN) hosts in the sample show additional and significant central suppression of [C II]/TIR, but these deficit enhancements occur not in those AGNs with the highest X-ray luminosities, but instead those with the highest central starlight intensities. Taken together, these results demonstrate that the [C II] line-cooling line deficit in galaxies likely arises from local physical phenomena in interstellar gas.

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KINGFISH—Key Insights on Nearby Galaxies: A Far-Infrared Survey withHerschel: Survey Description and Image Atlas1

Cited by 389 publications

References 154 publications

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

The Star Formation in Radio Survey: Jansky Very Large Array 33 GHz Observations of Nearby Galaxy Nuclei and Extranuclear Star-forming Regions

The Spatially Resolved Cooling Line Deficit in Galaxies

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KINGFISH—Key Insights on Nearby Galaxies: A Far-Infrared Survey withHerschel: Survey Description and Image Atlas1

Cited by 389 publications

References 154 publications

The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

The Star Formation in Radio Survey: Jansky Very Large Array 33 GHz Observations of Nearby Galaxy Nuclei and Extranuclear Star-forming Regions

The Spatially Resolved Cooling Line Deficit in Galaxies

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The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3