Star Formation in NGC 5194 (M51a): The Panchromatic View from<i>GALEX</i>to<i>Spitzer</i>

Calzetti, Daniela; Kennicutt, Robert C.; Bianchi, Luciana; Thilker, David A.; Dale, Daniel A.; Engelbracht, C. W.; Leitherer, Claus; Meyer, M.; Sosey, M.; Mutchler, Max; Regan, Michael W.; Thornley, M. D.; Armus, L.; Bendo, G. J.; Boissier, S.; Boselli, A.; Draine, B. T.; Gordon, K. D.; Hélou, G.; Hollenbach, D. J.; Kewley, Lisa J.; Madore, Barry F.; Martin, D. Christopher; Murphy, E. J.; Rieke, G. H.; Rieke, M. J.; Roussel, Hervé; Sheth, Kartik; Smith, John David; Walter, Fabian; White, Benjamin Thomas; Yi, Sukyoung K.; Scoville, N. Z.; Polletta, M.; Lindler, D. J.

doi:10.1086/466518

Cited by 402 publications

(637 citation statements)

References 97 publications

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“…Offsets and anti-correlations between FUV and 12 CO (or FIR and Hi) emissions have also been seen in other spiral galaxies such as M 100 (Rand 1995;Sempere & García-Burillo 1997;Calzetti et al 2005), M 51 (Calzetti et al 2005), and NGC 3147 (Casasola et al 2008a). These anti-correlations may relate to star formation efficiency and timescale variations in response to a spiral density wave.…”

Section: Far-ultraviolet Morphologymentioning

confidence: 74%

Molecular Gas in NUclei of GAlaxies (NUGA)

Casasola

Hunt

Combes

et al. 2011

A&A

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We present 12 CO(1-0) and 12 CO(2-1) maps of the interacting barred LINER/Seyfert 2 galaxy NGC 3627 obtained with the IRAM interferometer at resolutions of 2. 1 × 1. 3 and 0. 9 × 0. 6, respectively. We also present single-dish IRAM 30 m 12 CO(1-0) and 12 CO(2-1) observations used to compute short spacings and complete interferometric measurements. These observations are complemented by IRAM 30 m measurements of HCN(1-0) emission detected in the center of NGC 3627. The molecular gas emission shows a nuclear peak, an elongated bar-like structure of ∼18 (∼900 pc) diameter in both 12 CO maps and, in 12 CO(1-0), a two-arm spiral feature from r ∼ 9 (∼450 pc) to r ∼ 16 (∼800 pc). The inner ∼18 bar-like structure, with a north/south orientation (PA = 14 • ), forms two peaks at the extremes of this elongated emission region. The kinematics of the inner molecular gas shows signatures of non-circular motions associated both with the 18 bar-like structure and the spiral feature detected beyond it. The 1.6 μm H-band 2MASS image of NGC 3627 shows a stellar bar with a PA = −21 • , different from the PA (= 14 • ) of the 12 CO bar-like structure, indicating that the gas is leading the stellar bar. The far-infrared Spitzer-MIPS 70 and 160 μm images of NGC 3627 show that the dust emission is intensified at the nucleus and at the ansae at the ends of the bar, coinciding with the 12 CO peaks. The GALEX far-ultraviolet (FUV) morphology of NGC 3627 displays an inner elongated (north/south) ring delimiting a hole around the nucleus, and the 12 CO bar-like structure is contained in the hole observed in the FUV. The torques computed with the HST-NICMOS F160W image and our PdBI maps are negative down to the resolution limit of our images, ∼60 pc in 12 CO(2-1). If the bar ends at ∼3 kpc, coincident with corotation (CR), the torques are negative between the CR of the bar and the nucleus, down to the resolution limit of our observations. This scenario is compatible with a recently-formed rapidly rotating bar which has had insufficient time to slow down because of secular evolution, and thus has not yet formed an inner Lindblad resonance (ILR). The presence of molecular gas inside the CR of the primary bar, where we expect that the ILR will form, makes NGC 3627 a potential smoking gun of inner gas inflow. The gas is fueling the central region, and in a second step could fuel directly the active nucleus.

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Section: Far-ultraviolet Morphologymentioning

confidence: 74%

Molecular Gas in NUclei of GAlaxies (NUGA)

Casasola

Hunt

Combes

et al. 2011

A&A

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“…As part of SINGS (Spitzer Infrared Nearby Galaxies Survey, Kennicutt et al (2003)), Spitzer obtained high-resolution IR maps of a large sample of nearby galaxies. Calzetti et al (2005) and Calzetti et al (2007) demonstrated the utility of these maps to trace recently formed stars obscured on small scales, particularly when used in combination with Hα -a tracer of unobscured star formation.…”

Section: Recent Advances: Gas and Star Formation On Sub-kiloparsec Scmentioning

confidence: 99%

Scaling Relations between Gas and Star Formation in Nearby Galaxies

Bigiel¹,

Leroy

Walter

2010

Proc. IAU

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Abstract. High resolution, multi-wavelength maps of a sizeable set of nearby galaxies have made it possible to study how the surface densities of H i, H2 and star formation rate (ΣHI,ΣH2 ,ΣSFR ) relate on scales of a few hundred parsecs. At these scales, individual galaxy disks are comfortably resolved, making it possible to assess gas-SFR relations with respect to environment within galaxies. Σ H 2 , traced by CO intensity, shows a strong correlation with ΣSFR and the ratio between these two quantities, the molecular gas depletion time, appears to be constant at about 2 Gyr in large spiral galaxies. Within the star-forming disks of galaxies, ΣSFR shows almost no correlation with ΣHI. In the outer parts of galaxies, however, ΣSFR does scale with ΣHI, though with large scatter. Combining data from these different environments yields a distribution with multiple regimes in Σgas − ΣSFR space. If the underlying assumptions to convert observables to physical quantities are matched, even combined datasets based on different SFR tracers, methodologies and spatial scales occupy a well define locus in Σgas − ΣSFR space.

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“…The 8 µm mid-infrared emission is generally considered to trace the PAHs heated by UV photons (Leger & Puget 1984;Sellgren 1984). It is thought that 2/3 of the 8 µm emission from a galaxy originates from heating by stellar populations 100 Myr or younger (Calzetti et al 2005;Calzetti 2013), and that PAH emission is stronger for increasing metallicity and dust content of the interstellar medium (e.g., Engelbracht et al 2005;Marble et al 2010;Calzetti 2013). The 24 µm emission is generally produced by dust following absorption of UV photons emitted by young stars, and traces SF on a time scale of 10 Myr (Calzetti et al 2005;Leroy et al 2008).…”

Section: Ancillary Optical and Infrared Imagesmentioning

confidence: 99%

“…It is thought that 2/3 of the 8 µm emission from a galaxy originates from heating by stellar populations 100 Myr or younger (Calzetti et al 2005;Calzetti 2013), and that PAH emission is stronger for increasing metallicity and dust content of the interstellar medium (e.g., Engelbracht et al 2005;Marble et al 2010;Calzetti 2013). The 24 µm emission is generally produced by dust following absorption of UV photons emitted by young stars, and traces SF on a time scale of 10 Myr (Calzetti et al 2005;Leroy et al 2008). In this paper we use archival 3.6 µm, 8 µm and 24µm images from Fazio et al (2004) obtained with the Infrared Array Camera and The Multiband Imaging Photometer on the Spitzer Space Telescope (Rieke et al 2004;Werner et al 2004).…”

Section: Ancillary Optical and Infrared Imagesmentioning

confidence: 99%

“…2). In particular, we know that the PAH molecules traced by the 8 µm emission are vunerable to highly energetic photons in dust poor environments due to low dust shielding (e.g., Boselli, Lequeux & Gavazzi 2004;Calzetti et al 2005), and the PAH emission generally vanishes in regions with metallicity below solar (Engelbracht et al 2005). Thus the metallicity in the inner region should be significantly higher than in the outer regions.…”

Section: Star Formation Efficiencymentioning

confidence: 99%

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Star formation in the outer regions of the early-type galaxy NGC 4203

Yıldız¹,

Serra

Oosterloo

et al. 2015

Monthly Notices of the Royal Astronomical Society

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NGC 4203 is a nearby early-type galaxy surrounded by a very large, low-column-density H i disc. In this paper we study the star formation efficiency in the gas disc of NGC 4203 by using the UV, deep optical imaging and infrared data. We confirm that the H i disc consists of two distinct components: an inner star forming ring with radius from ∼1 to ∼3 R e f f , and an outer disc. The outer H i disc is 9 times more massive than the inner H i ring. At the location of the inner H i ring we detect spiral-like structure both in the deep g − r image and in the 8 µm Spitzer-IRAC image, extending in radius up to ∼ 3 R e f f . These two gas components have a different star formation efficiency likely due to the different metallicity and dust content. The inner component has a star formation efficiency very similar to the inner regions of late-type galaxies. Although the outer component has a very low star formation efficiency, it is similar to that of the outer regions of spiral galaxies and dwarfs. We suggest that these differences can be explained with different gas origins for the two components such as stellar mass loss for the inner H i ring and accretion from the inter galactic medium (IGM) for the outer H i disc. The low level star formation efficiency in the outer H i disc is not enough to change the morphology of NGC 4203, making the depletion time of the H i gas much too long.

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Star Formation in NGC 5194 (M51a): The Panchromatic View fromGALEXtoSpitzer

Abstract: Far ultraviolet to far infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Tele-1 Based on observations obtained with the Spitzer Space Telescope and with GALEX.

Cited by 402 publications

References 97 publications

Molecular Gas in NUclei of GAlaxies (NUGA)

Molecular Gas in NUclei of GAlaxies (NUGA)

Scaling Relations between Gas and Star Formation in Nearby Galaxies

Star formation in the outer regions of the early-type galaxy NGC 4203

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