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Start Over Author "Kennicutt R. C." Journal monthly notices of the royal astronomical society
32 results on '"Kennicutt R. C."'

1. Fraction of stars in clusters for the LEGUS dwarf galaxies

Author

Cook, D O, primary, Lee, J C, additional, Adamo, A, additional, Calzetti, D, additional, Chandar, R, additional, Whitmore, B C, additional, Aloisi, A, additional, Cignoni, M, additional, Dale, D A, additional, Elmegreen, B G, additional, Fumagalli, M, additional, Grasha, K, additional, Johnson, K E, additional, Kennicutt, R C, additional, Kim, H, additional, Linden, S T, additional, Messa, M, additional, Östlin, G, additional, Ryon, J E, additional, Sacchi, E, additional, Thilker, D A, additional, Tosi, M, additional, and Wofford, A, additional

Published
2022
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2. Fraction of stars in clusters for the LEGUS dwarf galaxies.

Author

Cook, D O, Lee, J C, Adamo, A, Calzetti, D, Chandar, R, Whitmore, B C, Aloisi, A, Cignoni, M, Dale, D A, Elmegreen, B G, Fumagalli, M, Grasha, K, Johnson, K E, Kennicutt, R C, Kim, H, Linden, S T, Messa, M, Östlin, G, Ryon, J E, and Sacchi, E

Subjects
STELLAR populations, STAR formation, GALAXY clusters, GALAXY formation, STAR clusters, SPACE telescopes, DWARF galaxies
Abstract

We study the young star cluster populations in 23 dwarf and irregular galaxies observed by the Hubble Space Telescope (HST) Legacy ExtraGalactic Ultraviolet Survey (LEGUS), and examine relationships between the ensemble properties of the cluster populations and those of their host galaxies: star formation rate (SFR) density (ΣSFR). A strength of this analysis is the availability of SFRs measured from temporally resolved star formation histories that provide the means to match cluster and host galaxy properties on several time-scales (1–10, 1–100, and 10–100 Myr). Nevertheless, studies of this kind are challenging for dwarf galaxies due to the small numbers of clusters in each system. We mitigate these issues by combining the clusters across different galaxies with similar ΣSFR properties. We find good agreement with a well-established relationship (⁠|$M_{V}^{\mathrm{ brightest}}$| –SFR), but find no significant correlations between ΣSFR and the slopes of the cluster luminosity function, mass function, nor the age distribution. We also find no significant trend between the fraction of stars in bound clusters at different age ranges (Γ1–10, Γ10–100, and Γ1–100) and ΣSFR of the host galaxy. Our data show a decrease in Γ over time (from 1–10 to 10–100 Myr) suggesting early cluster dissolution, though the presence of unbound clusters in the youngest time bin makes it difficult to quantify the degree of dissolution. While our data do not exhibit strong correlations between ΣSFR and ensemble cluster properties, we cannot rule out that a weak trend might exist given the relatively large uncertainties due to low number statistics and the limited ΣSFR range probed. [ABSTRACT FROM AUTHOR]

Published
2023
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3. LeMMINGs – II. The e-MERLIN legacy survey of nearby galaxies. The deepest radio view of the Palomar sample on parsec scale

Author

Baldi, R D, primary, Williams, D R A, additional, McHardy, I M, additional, Beswick, R J, additional, Brinks, E, additional, Dullo, B T, additional, Knapen, J H, additional, Argo, M K, additional, Aalto, S, additional, Alberdi, A, additional, Baan, W A, additional, Bendo, G J, additional, Corbel, S, additional, Fenech, D M, additional, Gallagher, J S, additional, Green, D A, additional, Kennicutt, R C, additional, Klöckner, H-R, additional, Körding, E, additional, Maccarone, T J, additional, Muxlow, T W B, additional, Mundell, C G, additional, Panessa, F, additional, Peck, A B, additional, Pérez-Torres, M A, additional, Romero-Cañizales, C, additional, Saikia, P, additional, Shankar, F, additional, Spencer, R E, additional, Stevens, I R, additional, Varenius, E, additional, Ward, M J, additional, Yates, J, additional, and Uttley, P, additional

Published
2020
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4. JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

Author

De Looze, I, primary, Lamperti, I, primary, Saintonge, A, primary, Relaño, M, primary, Smith, M W L, primary, Clark, C J R, primary, Wilson, C D, primary, Decleir, M, primary, Jones, A P, primary, Kennicutt, R C, primary, Accurso, G, primary, Brinks, E, primary, Bureau, M, primary, Cigan, P, primary, Clements, D L, primary, De Vis, P, primary, Fanciullo, L, primary, Gao, Y, primary, Gear, W K, primary, Ho, L C, primary, Hwang, H S, primary, Michałowski, M J, primary, Lee, J C, primary, Li, C, primary, Lin, L, primary, Liu, T, primary, Lomaeva, M, primary, Pan, H-A, primary, Sargent, M, primary, Williams, T, primary, Xiao, T, primary, and Zhu, M, primary

Published
2020
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5. SIGNALS: I. Survey description

Author

Rousseau-Nepton, L, primary, Martin, R P, additional, Robert, C, additional, Drissen, L, additional, Amram, P, additional, Prunet, S, additional, Martin, T, additional, Moumen, I, additional, Adamo, A, additional, Alarie, A, additional, Barmby, P, additional, Boselli, A, additional, Bresolin, F, additional, Bureau, M, additional, Chemin, L, additional, Fernandes, R C, additional, Combes, F, additional, Crowder, C, additional, Della Bruna, L, additional, Duarte Puertas, S, additional, Egusa, F, additional, Epinat, B, additional, Ksoll, V F, additional, Girard, M, additional, Gómez Llanos, V, additional, Gouliermis, D, additional, Grasha, K, additional, Higgs, C, additional, Hlavacek-Larrondo, J, additional, Ho, I-T, additional, Iglesias-Páramo, J, additional, Joncas, G, additional, Kam, Z S, additional, Karera, P, additional, Kennicutt, R C, additional, Klessen, R S, additional, Lianou, S, additional, Liu, L, additional, Liu, Q, additional, de Amorim, A Luiz, additional, Lyman, J D, additional, Martel, H, additional, Mazzilli-Ciraulo, B, additional, McLeod, A F, additional, Melchior, A-L, additional, Millan, I, additional, Mollá, M, additional, Momose, R, additional, Morisset, C, additional, Pan, H-A, additional, Pati, A K, additional, Pellerin, A, additional, Pellegrini, E, additional, Pérez, I, additional, Petric, A, additional, Plana, H, additional, Rahner, D, additional, Ruiz Lara, T, additional, Sánchez-Menguiano, L, additional, Spekkens, K, additional, Stasińska, G, additional, Takamiya, M, additional, Vale Asari, N, additional, and Vílchez, J M, additional

Published
2019
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6. Star cluster catalogues for the LEGUS dwarf galaxies

Author

Cook, D O, primary, Lee, J C, additional, Adamo, A, additional, Kim, H, additional, Chandar, R, additional, Whitmore, B C, additional, Mok, A, additional, Ryon, J E, additional, Dale, D A, additional, Calzetti, D, additional, Andrews, J E, additional, Aloisi, A, additional, Ashworth, G, additional, Bright, S N, additional, Brown, T M, additional, Christian, C, additional, Cignoni, M, additional, Clayton, G C, additional, da Silva, R, additional, de Mink, S E, additional, Dobbs, C L, additional, Elmegreen, B G, additional, Elmegreen, D M, additional, Evans, A S, additional, Fumagalli, M, additional, Gallagher, J S, additional, Gouliermis, D A, additional, Grasha, K, additional, Grebel, E K, additional, Herrero, A, additional, Hunter, D A, additional, Jensen, E I, additional, Johnson, K E, additional, Kahre, L, additional, Kennicutt, R C, additional, Krumholz, M R, additional, Lee, N J, additional, Lennon, D, additional, Linden, S, additional, Martin, C, additional, Messa, M, additional, Nair, P, additional, Nota, A, additional, Östlin, G, additional, Parziale, R C, additional, Pellerin, A, additional, Regan, M W, additional, Sabbi, E, additional, Sacchi, E, additional, Schaerer, D, additional, Schiminovich, D, additional, Shabani, F, additional, Slane, F A, additional, Small, J, additional, Smith, C L, additional, Smith, L J, additional, Taibi, S, additional, Thilker, D A, additional, de la Torre, I C, additional, Tosi, M, additional, Turner, J A, additional, Ubeda, L, additional, Van Dyk, S D, additional, Walterbos, R AM, additional, and Wofford, A, additional

Published
2019
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7. The spatial relation between young star clusters and molecular clouds in M51 with LEGUS

Author

Grasha, K, primary, Calzetti, D, additional, Adamo, A, additional, Kennicutt, R C, additional, Elmegreen, B G, additional, Messa, M, additional, Dale, D A, additional, Fedorenko, K, additional, Mahadevan, S, additional, Grebel, E K, additional, Fumagalli, M, additional, Kim, H, additional, Dobbs, C L, additional, Gouliermis, D A, additional, Ashworth, G, additional, Gallagher, J S, additional, Smith, L J, additional, Tosi, M, additional, Whitmore, B C, additional, Schinnerer, E, additional, Colombo, D, additional, Hughes, A, additional, Leroy, A K, additional, and Meidt, S E, additional

Published
2018
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8. Connecting young star clusters to CO molecular gas in NGC 7793 with ALMA–LEGUS

Author

Grasha, K, primary, Calzetti, D, additional, Bittle, L, additional, Johnson, K E, additional, Donovan Meyer, J, additional, Kennicutt, R C, additional, Elmegreen, B G, additional, Adamo, A, additional, Krumholz, M R, additional, Fumagalli, M, additional, Grebel, E K, additional, Gouliermis, D A, additional, Cook, D O, additional, Gallagher, J S, additional, Aloisi, A, additional, Dale, D A, additional, Linden, S, additional, Sacchi, E, additional, Thilker, D A, additional, Walterbos, R A M, additional, Messa, M, additional, Wofford, A, additional, and Smith, L J, additional

Published
2018
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9. Near-identical star formation rate densities from Hα and FUVat redshift zero

Author

Audcent-Ross, Fiona M, primary, Meurer, Gerhardt R, additional, Wong, O I, additional, Zheng, Z, additional, Hanish, D, additional, Zwaan, M A, additional, Bland-Hawthorn, J, additional, Elagali, A, additional, Meyer, M, additional, Putman, M E, additional, Ryan-Weber, E V, additional, Sweet, S M, additional, Thilker, D A, additional, Seibert, M, additional, Allen, R, additional, Dopita, M A, additional, Doyle-Pegg, M T, additional, Drinkwater, M, additional, Ferguson, H C, additional, Freeman, K C, additional, Heckman, T M, additional, Kennicutt, R C, additional, Kilborn, V A, additional, Kim, J H, additional, Knezek, P M, additional, Koribalski, B, additional, Smith, R C, additional, Staveley-Smith, L, additional, Webster, R L, additional, and Werk, J K, additional

Published
2018
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10. spatial relation between young star clusters and molecular clouds in M51 with LEGUS.

Author

Grasha, K, Calzetti, D, Adamo, A, Kennicutt, R C, Elmegreen, B G, Messa, M, Dale, D A, Fedorenko, K, Mahadevan, S, Grebel, E K, Fumagalli, M, Kim, H, Dobbs, C L, Gouliermis, D A, Ashworth, G, Gallagher, J S, Smith, L J, Tosi, M, Whitmore, B C, and Schinnerer, E

Subjects
STAR clusters, MOLECULAR clouds, STELLAR evolution, STARBURSTS, STELLAR density (Stellar population)
Abstract

We present a study correlating the spatial locations of young star clusters with those of molecular clouds in NGC 5194, in order to investigate the time-scale over which clusters separate from their birth clouds. The star cluster catalogues are from the Legacy ExtraGalactic UV Survey (LEGUS) and the molecular clouds from the Plateau de Bure Interefrometer Arcsecond Whirpool Survey (PAWS). We find that younger star clusters are spatially closer to molecular clouds than older star clusters. The median age for clusters associated with clouds is 4 Myr, whereas it is 50 Myr for clusters that are sufficiently separated from a molecular cloud to be considered unassociated. After ∼6 Myr, the majority of the star clusters lose association with their molecular gas. Younger star clusters are also preferentially located in stellar spiral arms where they are hierarchically distributed in kpc-size regions for 50–100 Myr before dispersing. The youngest star clusters are more strongly clustered, yielding a two-point correlation function with α = −0.28 ± 0.04, than the giant molecular cloud (GMCs) (α = −0.09 ± 0.03) within the same PAWS field. However, the clustering strength of the most massive GMCs, supposedly the progenitors of the young clusters for a star formation efficiency of a few per cent, is comparable (α = −0.35 ± 0.05) to that of the clusters. We find a galactocentric dependence for the coherence of star formation, in which clusters located in the inner region of the galaxy reside in smaller star-forming complexes and display more homogeneous distributions than clusters further from the centre. This result suggests a correlation between the survival of a cluster complex and its environment. [ABSTRACT FROM AUTHOR]

Published
2019
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13. Calibration of the total infrared luminosity of nearby galaxies from Spitzer and Herschel bands

Author

Galametz, M., primary, Kennicutt, R. C., additional, Calzetti, D., additional, Aniano, G., additional, Draine, B. T., additional, Boquien, M., additional, Brandl, B., additional, Croxall, K. V., additional, Dale, D. A., additional, Engelbracht, C. W., additional, Gordon, K. D., additional, Groves, B., additional, Hao, C.-N., additional, Helou, G., additional, Hinz, J. L., additional, Hunt, L. K., additional, Johnson, B. D., additional, Li, Y., additional, Murphy, E., additional, Roussel, H., additional, Sandstrom, K., additional, Skibba, R. A., additional, and Tabatabaei, F. S., additional

Published
2013
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14. Mapping the cold dust temperatures and masses of nearby KINGFISH galaxies withHerschel

Author

Galametz, M., primary, Kennicutt, R. C., additional, Albrecht, M., additional, Aniano, G., additional, Armus, L., additional, Bertoldi, F., additional, Calzetti, D., additional, Crocker, A. F., additional, Croxall, K. V., additional, Dale, D. A., additional, Donovan Meyer, J., additional, Draine, B. T., additional, Engelbracht, C. W., additional, Hinz, J. L., additional, Roussel, H., additional, Skibba, R. A., additional, Tabatabaei, F. S., additional, Walter, F., additional, Weiss, A., additional, Wilson, C. D., additional, and Wolfire, M. G., additional

Published
2012
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17. The evolution of stellar structures in dwarf galaxies

Author

Bastian, N., primary, Weisz, D. R., additional, Skillman, E. D., additional, McQuinn, K. B. W., additional, Dolphin, A. E., additional, Gutermuth, R. A., additional, Cannon, J. M., additional, Ercolano, B., additional, Gieles, M., additional, Kennicutt, R. C., additional, and Walter, F., additional

Published
2011
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21. PINGS: the PPAK IFS Nearby Galaxies Survey

Author

Rosales-Ortega, F. F., primary, Kennicutt, R. C., additional, Sánchez, S. F., additional, Díaz, A. I., additional, Pasquali, A., additional, Johnson, B. D., additional, and Hao, C. N., additional

Published
2010
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27. NGC 922 - a new drop-through ring galaxy★

Author

Wong, O. I., primary, Meurer, G. R., additional, Bekki, K., additional, Hanish, D. J., additional, Kennicutt, R. C., additional, Bland-Hawthorn, J., additional, Ryan-Weber, E. V., additional, Koribalski, B., additional, Kilborn, V. A., additional, Putman, M. E., additional, Heiner, J. S., additional, Webster, R. L., additional, Allen, R. J., additional, Dopita, M. A., additional, Doyle, M. T., additional, Drinkwater, M. J., additional, Ferguson, H. C., additional, Freeman, K. C., additional, Heckman, T. M., additional, Hoopes, C., additional, Knezek, P. M., additional, Meyer, M. J., additional, Oey, M. S., additional, Seibert, M., additional, Smith, R. C., additional, Staveley-Smith, L., additional, Thilker, D., additional, Werk, J., additional, and Zwaan, M. A., additional

Published
2006
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29. On how leakage can affect the star formation rate estimation using Hα luminosity.

Author

Relaño, M., Kennicutt, R. C., Eldridge, J. J., Lee, J. C., and Verley, S.

Subjects
*STAR formation, *STELLAR luminosity function, *GALAXY clusters, *EXPANDING universe, *MAGELLANIC clouds, *EINSTEIN-Podolsky-Rosen experiment
Abstract

We present observational evidence that leakage of ionizing photons from star-forming regions can affect the quantification of the star formation rate (SFR) in galaxies. This effect could partially explain the differences between the SFR estimates using the far-ultraviolet (FUV) and the Hα emission. We find that leakage could decrease the SFR(Hα)/SFR(FUV) ratio by up to 25 per cent. The evidence is based on the observation that the SFR(Hα)/SFR(FUV) ratio is lower for objects showing a shell Hα structure than for regions exhibiting a much more compact morphology. The study has been performed on three object samples: low-luminosity dwarf galaxies from the Local Volume Legacy survey, star-forming regions in the Large Magellanic Cloud and the nearby Local Group galaxy M33. For the three samples we find differences (1.1σ–1.4σ) between the SFR(Hα)/SFR(FUV) for compact and shell objects. Although leakage cannot entirely explain the observed trend of SFR(Hα)/SFR(FUV) ratios for systems with low SFR, we show that the mechanism can lead to different SFR estimates when using Hα and FUV luminosities. Therefore, further study is needed to constrain the contribution of leakage to the low SFR(Hα)/SFR(FUV) ratios observed in dwarf galaxies and its impact on the Hα flux as an SFR indicator in such objects. [ABSTRACT FROM AUTHOR]

Published
2012

30. On the nature of the H.

Author

Goddard, Q. E., Bresolin, F., Kennicutt, R. C., Ryan-Weber, E. V., and Rosales-Ortega, F. F.

Subjects
HYDROGEN, GALAXY spectra, SPECTROGRAPHS, COSMIC abundances, DISKS (Astrophysics), STELLAR populations, STELLAR mass
Abstract

Using deep Subaru/Faint Object Camera And Spectrograph (FOCAS) spectra of 34 H regions in both the inner and outer parts of the extended ultraviolet (XUV) disc galaxy NGC 4625 we have measured an abundance gradient out to almost 2.5 times the optical isophotal radius. We applied several strong line abundance calibrations to determine the H region abundances, including , [N ]/[O ], [N ]/H as well as the [O ]4363 auroral line, which we detected in three of the H regions. We find that at the transition between the inner and outer disc the abundance gradient becomes flatter. In addition, there appears to be an abundance discontinuity in proximity of this transition. Several of our target H regions appear to deviate from the ionization sequence defined in the [N ]/H versus [O ]/H diagnostic diagram by bright extragalactic H regions. Using theoretical models we conclude that the most likely explanations for these deviations are either related to the time evolution of the H regions or stochastic variations in the ionizing stellar populations of these low-mass H regions, although we are unable to distinguish between these two effects. Such effects can also impact on the reliability of the strong line abundance determinations. [ABSTRACT FROM AUTHOR]

Published
2011
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31. PPAK Wide-field Integral Field Spectroscopy of NGC 628 - I. The largest spectroscopic mosaic on a single galaxy.

Author

Sánchez, S. F., Rosales-Ortega, F. F., Kennicutt, R. C., Johnson, B. D., Diaz, A. I., Pasquali, A., and Hao, C. N.

Subjects
INTEGRAL field spectroscopy, GALAXIES, ASTRONOMICAL observations, CALIBRATION, SPECTROPHOTOMETRY, STELLAR luminosity function, COSMIC abundances, STAR formation, STELLAR populations
Abstract

We present a wide-field Integral Field Spectroscopy (IFS) survey on the nearby face-on Sbc galaxy NGC 628, comprising 11094 individual spectra, covering a nearly circular field-of-view of ∼6 arcmin in diameter, with a sampling of ∼2.7 arcsec per spectrum in the optical wavelength range (3700-7000 Å). This galaxy is part of the PPAK IFS Nearby Galaxies Survey (PINGS). To our knowledge, this is the widest spectroscopic survey ever made in a single nearby galaxy. A detailed flux calibration was applied, granting a spectrophotometric accuracy of ∼0.2 mag. The spectroscopic data were analysed both as a single integrated spectrum that characterizes the global properties of the galaxy and using each individual spectrum to determine the spatial variation of the stellar and ionized gas components. The spatial distribution of the luminosity-weighted ages and metallicities of the stellar populations was analysed. Using typical strong emission-line ratios we derived the integrated and 2D spatial distribution of the ionized gas, the dust content, star formation rate (SFR) and oxygen abundance. The age of the stellar populations shows a negative gradient from the inner (older) to the outer (younger) regions. We found an inversion of this gradient in the central ∼1 kpc region, where a somewhat younger stellar population is present within a ring at this radius. This structure is associated with a circumnuclear star-forming region at ∼500 pc, also found in similar spiral galaxies. From the study of the integrated and spatially resolved ionized gas, we found a moderate SFR of . The oxygen abundance shows a clear gradient of higher metallicity values from the inner part to the outer part of the galaxy, with a mean value of 12 + log(O/H) ∼ 8.7. At some specific regions of the galaxy, the spatially resolved distribution of the physical properties shows some level of structure, suggesting real point-to-point variations within an individual H region. Our results are consistent with an inside-out growth scheme, with stronger star formation at the outer regions, and with evolved stellar populations in the inner ones. [ABSTRACT FROM AUTHOR]

Published
2011
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