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  • 1
    Online Resource
    Online Resource
    American Society of Colon and Rectal Surgeons 91st Annual Convention Podium and Poster abstracts : June 7-12, 1992 San Francisco, CA
    Ovid Technologies (Wolters Kluwer Health) ; 1992
    In:  Diseases of the Colon & Rectum Vol. 35, No. 5 ( 1992-05), p. 1-45
    Details
    In: Diseases of the Colon & Rectum, Ovid Technologies (Wolters Kluwer Health), Vol. 35, No. 5 ( 1992-05), p. 1-45
    Type of Medium: Online Resource
    ISSN: 0012-3706
    URL: Article
    DOI: 10.1007/BF02049421
    Language: English
    Publisher: Ovid Technologies (Wolters Kluwer Health)
    Publication Date: 1992
    detail.hit.zdb_id: 2046914-7
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  • 2
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    Stellar structures, molecular gas, and star formation across the PHANGS sample of nearby galaxies
    EDP Sciences ; 2021
    In:  Astronomy & Astrophysics Vol. 656 ( 2021-12), p. A133-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 656 ( 2021-12), p. A133-
    Abstract: We identify stellar structures in the PHANGS sample of 74 nearby galaxies and construct morphological masks of sub-galactic environments based on Spitzer 3.6  μ m images. At the simplest level, we distinguish five environments: centres, bars, spiral arms, interarm regions, and discs without strong spirals. Slightly more sophisticated masks include rings and lenses, which are publicly released but not explicitly used in this paper. We examine trends with environment in the molecular gas content, star formation rate, and depletion time using PHANGS–ALMA CO(2–1) intensity maps and tracers of star formation. The interarm regions and discs without strong spirals clearly dominate in area, whereas molecular gas and star formation are quite evenly distributed among the five basic environments. We reproduce the molecular Kennicutt–Schmidt relation with a slope compatible with unity within the uncertainties and without significant slope differences among environments. In contrast to what has been suggested by early studies, we find that bars are not always deserts devoid of gas and star formation, but instead they show large diversity. Similarly, spiral arms do not account for most of the gas and star formation in disc galaxies, and they do not have shorter depletion times than the interarm regions. Spiral arms accumulate gas and star formation, without systematically boosting the star formation efficiency. Centres harbour remarkably high surface densities and on average shorter depletion times than other environments. Centres of barred galaxies show higher surface densities and wider distributions compared to the outer disc; yet, depletion times are similar to unbarred galaxies, suggesting highly intermittent periods of star formation when bars episodically drive gas inflow, without enhancing the central star formation efficiency permanently. In conclusion, we provide quantitative evidence that stellar structures in galaxies strongly affect the organisation of molecular gas and star formation, but their impact on star formation efficiency is more subtle.
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/202140695
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2021
    detail.hit.zdb_id: 1458466-9
    SSG: 16,12
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  • 3
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    Online Resource
    Star formation scaling relations at ∼100 pc from PHANGS: Impact of completeness and spatial scale
    EDP Sciences ; 2021
    In:  Astronomy & Astrophysics Vol. 650 ( 2021-06), p. A134-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 650 ( 2021-06), p. A134-
    Abstract: Aims. The complexity of star formation at the physical scale of molecular clouds is not yet fully understood. We investigate the mechanisms regulating the formation of stars in different environments within nearby star-forming galaxies from the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) sample. Methods. Integral field spectroscopic data and radio-interferometric observations of 18 galaxies were combined to explore the existence of the resolved star formation main sequence (Σ stellar versus Σ SFR ), resolved Kennicutt–Schmidt relation (Σ mol. gas versus Σ SFR ), and resolved molecular gas main sequence (Σ stellar versus Σ mol. gas ), and we derived their slope and scatter at spatial resolutions from 100 pc to 1 kpc (under various assumptions). Results. All three relations were recovered at the highest spatial resolution (100 pc). Furthermore, significant variations in these scaling relations were observed across different galactic environments. The exclusion of non-detections has a systematic impact on the inferred slope as a function of the spatial scale. Finally, the scatter of the Σ mol. gas + stellar versus Σ SFR correlation is smaller than that of the resolved star formation main sequence, but higher than that found for the resolved Kennicutt–Schmidt relation. Conclusions. The resolved molecular gas main sequence has the tightest relation at a spatial scale of 100 pc (scatter of 0.34 dex), followed by the resolved Kennicutt–Schmidt relation (0.41 dex) and then the resolved star formation main sequence (0.51 dex). This is consistent with expectations from the timescales involved in the evolutionary cycle of molecular clouds. Surprisingly, the resolved Kennicutt–Schmidt relation shows the least variation across galaxies and environments, suggesting a tight link between molecular gas and subsequent star formation. The scatter of the three relations decreases at lower spatial resolutions, with the resolved Kennicutt–Schmidt relation being the tightest (0.27 dex) at a spatial scale of 1 kpc. Variation in the slope of the resolved star formation main sequence among galaxies is partially due to different detection fractions of Σ SFR with respect to Σ stellar .
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/202140733
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2021
    detail.hit.zdb_id: 1458466-9
    SSG: 16,12
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  • 4
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    Variations in the Σ SFR  − Σ mol  − Σ ⋆ plane across galactic environments in PHANGS galaxies
    EDP Sciences ; 2022
    In:  Astronomy & Astrophysics Vol. 663 ( 2022-07), p. A61-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 663 ( 2022-07), p. A61-
    Abstract: Aims. There exists some consensus that the stellar mass surface density (Σ ⋆ ) and molecular gas mass surface density (Σ mol ) are the main quantities responsible for locally setting the star formation rate. This regulation is inferred from locally resolved scaling relations between these two quantities and the star formation rate surface density (Σ SFR ), which have been extensively studied in a wide variety of works. However, the universality of these relations is debated. Here, we probe the interplay between these three quantities across different galactic environments at a spatial resolution of 150 pc. Methods. We performed a hierarchical Bayesian linear regression to find the best set of parameters C ⋆ , C mol , and C norm that describe the star-forming plane conformed by Σ ⋆ , Σ mol , and Σ SFR , such that logΣ SFR  =  C ⋆ logΣ ⋆  +  C mol logΣ mol  +  C norm . We also explored variations in the determined parameters across galactic environments, focusing our analysis on the C ⋆ and C mol slopes. Results. We find signs of variations in the posterior distributions of C ⋆ and C mol across different galactic environments. The dependence of Σ SFR on Σ ⋆ spans a wide range of slopes, with negative and positive values, while the dependence of Σ SFR on Σ mol is always positive. Bars show the most negative value of C ⋆ (−0.41), which is a sign of longer depletion times, while spiral arms show the highest C ⋆ among all environments (0.45). Variations in C mol also exist, although they are more subtle than those found for C ⋆ . Conclusions. We conclude that systematic variations in the interplay of Σ ⋆ , Σ mol , and Σ SFR across different galactic environments exist at a spatial resolution of 150 pc, and we interpret these variations to be produced by an additional mechanism regulating the formation of stars that is not captured by either Σ ⋆ or Σ mol . Studying environmental variations in single galaxies, we find that these variations correlate with changes in the star formation efficiency across environments, which could be linked to the dynamical state of the gas that prevents it from collapsing and forming stars, or to changes in the molecular gas fraction.
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/202142832
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2022
    detail.hit.zdb_id: 1458466-9
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  • 5
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    Kinematic analysis of the super-extended H I disk of the nearby spiral galaxy M 83
    EDP Sciences ; 2023
    In:  Astronomy & Astrophysics Vol. 675 ( 2023-07), p. A37-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 675 ( 2023-07), p. A37-
    Abstract: We present new H  I observations of the nearby massive spiral galaxy M 83 taken with the JVLA at 21″ angular resolution (≈500 pc) of an extended (∼1.5 deg 2 ) ten-point mosaic combined with GBT single-dish data. We study the super-extended H  I disk of M 83 (∼50 kpc in radius), in particular disk kinematics, rotation, and the turbulent nature of the atomic interstellar medium. We define distinct regions in the outer disk ( r gal 〉 central optical disk), including a ring, a southern area, a southern arm and a northern arm. We examine H  I gas surface density, velocity dispersion, and noncircular motions in the outskirts, which we compare to the inner optical disk. We find an increase of velocity dispersion ( σ v ) toward the pronounced H  I ring, indicative of more turbulent H  I gas. Additionally, we report over a large galactocentric radius range (until r gal  ∼ 50 kpc) where σ v is slightly larger than thermal component (i.e., 〉 8 km s −1 ). We find that a higher star-formation rate (as traced by far UV emission) is not necessarily always associated with a higher H  I velocity dispersion, suggesting that radial transport could be a dominant driver for the enhanced velocity dispersion. Furthermore, we find a possible branch that connects the extended H  I disk to the dwarf irregular galaxy UGCA 365 and that deviates from the general direction of the northern arm. Lastly, we compare mass flow rate profiles (based on 2D and 3D tilted ring models) and find evidence for outflowing gas at r gal ∼ 2 kpc, inflowing gas at r gal ∼ 5.5 kpc, and outflowing gas at r gal  ∼ 14 kpc. We caution that mass flow rates are highly sensitive to the assumed kinematic disk parameters, in particular to inclination.
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/202245290
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2023
    detail.hit.zdb_id: 1458466-9
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  • 6
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    Comparing the pre-SNe feedback and environmental pressures for 6000 H  ii regions across 19 nearby spiral galaxies
    Oxford University Press (OUP) ; 2021
    In:  Monthly Notices of the Royal Astronomical Society Vol. 508, No. 4 ( 2021-10-28), p. 5362-5389
    Details
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 508, No. 4 ( 2021-10-28), p. 5362-5389
    Abstract: The feedback from young stars (i.e. pre-supernova) is thought to play a crucial role in molecular cloud destruction. In this paper, we assess the feedback mechanisms acting within a sample of 5810 H ii regions identified from the PHANGS-MUSE survey of 19 nearby ( & lt;20 Mpc) star-forming, main-sequence spiral galaxies [log(M⋆/M⊙) = 9.4–11]. These optical spectroscopic maps are essential to constrain the physical properties of the H ii regions, which we use to investigate their internal pressure terms. We estimate the photoionized gas (Ptherm), direct radiation (Prad), and mechanical wind pressure (Pwind), which we compare to the confining pressure of their host environment (Pde). The H ii regions remain unresolved within our ∼50–100 pc resolution observations, so we place upper (Pmax) and lower (Pmin) limits on each of the pressures by using a minimum (i.e. clumpy structure) and maximum (i.e. smooth structure) size, respectively. We find that the Pmax measurements are broadly similar, and for Pmin the Ptherm is mildly dominant. We find that the majority of H ii regions are overpressured, Ptot/Pde = (Ptherm + Pwind + Prad)/Pde & gt; 1, and expanding, yet there is a small sample of compact H ii regions with Ptot,max/Pde & lt; 1 (∼1 per cent of the sample). These mostly reside in galaxy centres (Rgal & lt; 1 kpc), or, specifically, environments of high gas surface density; log(Σgas/M⊙ pc−2) ∼ 2.5 (measured on kpc-scales). Lastly, we compare to a sample of literature measurements for Ptherm and Prad to investigate how dominant pressure term transitions over around 5 dex in spatial dynamic range and 10 dex in pressure.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    URL: Article
    DOI: 10.1093/mnras/stab2958
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2021
    detail.hit.zdb_id: 2016084-7
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  • 7
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    Online Resource
    The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) : I. The UV luminosity function of the central 12 sq. deg
    EDP Sciences ; 2011
    In:  Astronomy & Astrophysics Vol. 528 ( 2011-4), p. A107-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 528 ( 2011-4), p. A107-
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/201016389
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2011
    detail.hit.zdb_id: 1458466-9
    SSG: 16,12
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  • 8
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    The PHANGS–MUSE nebular catalogue
    Oxford University Press (OUP) ; 2023
    In:  Monthly Notices of the Royal Astronomical Society Vol. 520, No. 4 ( 2023-02-22), p. 4902-4952
    Details
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 520, No. 4 ( 2023-02-22), p. 4902-4952
    Abstract: Ionized nebulae provide critical insights into the conditions of the interstellar medium (ISM). Their bright emission lines enable the measurement of physical properties, such as the gas-phase metallicity, across galaxy discs and in distant galaxies. The PHANGS–MUSE survey has produced optical spectroscopic coverage of the central star-forming discs of 19 nearby main-sequence galaxies. Here, we use the $\rm {H}\,\alpha$ morphology from this data to identify 30 790 distinct nebulae, finding thousands of nebulae per galaxy. For each nebula, we extract emission line fluxes and, using diagnostic line ratios, identify the dominant excitation mechanism. A total of 23 244 nebulae (75 per cent) are classified as H ii regions. The dust attenuation of every nebulae is characterized via the Balmer decrement and we use existing environmental masks to identify their large-scale galactic environment (centre, bar, arm, interarm, and disc). Using strong-line prescriptions, we measure the gas-phase oxygen abundances (metallicity) and ionization parameter for all H ii regions. With this new catalogue, we measure the radial metallicity gradients and explore second-order metallicity variations within each galaxy. By quantifying the global scatter in metallicity per galaxy, we find a weak negative correlation with global star formation rate and stronger negative correlation with global gas velocity dispersion (in both ionized and molecular gas). With this paper we release the full catalogue of strong line fluxes and derived properties, providing a rich data base for a broad variety of ISM studies.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    URL: Article
    DOI: 10.1093/mnras/stad114
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2023
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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  • 9
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    Erratum: “Mapping Metallicity Variations across Nearby Galaxy Disks” (2019, ApJ, 887, 80)
    American Astronomical Society ; 2021
    In:  The Astrophysical Journal Vol. 912, No. 2 ( 2021-05-01), p. 167-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 912, No. 2 ( 2021-05-01), p. 167-
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/abf7c2
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2021
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 10
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    Stellar feedback in a clumpy galaxy at z ∼ 3.4
    Oxford University Press (OUP) ; 2021
    In:  Monthly Notices of the Royal Astronomical Society Vol. 507, No. 3 ( 2021-09-09), p. 3830-3848
    Details
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 507, No. 3 ( 2021-09-09), p. 3830-3848
    Abstract: Giant star-forming regions (clumps) are widespread features of galaxies at z ≈ 1−4. Theory predicts that they can play a crucial role in galaxy evolution, if they survive to stellar feedback for & gt;50 Myr. Numerical simulations show that clumps’ survival depends on the stellar feedback recipes that are adopted. Up to date, observational constraints on both clumps’ outflows strength and gas removal time-scale are still uncertain. In this context, we study a line-emitting galaxy at redshift z ≃ 3.4 lensed by the foreground galaxy cluster Abell 2895. Four compact clumps with sizes ≲280 pc and representative of the low-mass end of clumps’ mass distribution (stellar masses ≲2 × 108 M⊙) dominate the galaxy morphology. The clumps are likely forming stars in a starbursting mode and have a young stellar population (∼10 Myr). The properties of the Lyman-α (Lyα) emission and nebular far-ultraviolet absorption lines indicate the presence of ejected material with global outflowing velocities of ∼200–300 km s−1. Assuming that the detected outflows are the consequence of star formation feedback, we infer an average mass loading factor (η) for the clumps of ∼1.8–2.4 consistent with results obtained from hydrodynamical simulations of clumpy galaxies that assume relatively strong stellar feedback. Assuming no gas inflows (semiclosed box model), the estimates of η suggest that the time-scale over which the outflows expel the molecular gas reservoir (≃7 × 108 M⊙) of the four detected low-mass clumps is ≲50 Myr.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    URL: Article
    DOI: 10.1093/mnras/stab2376
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2021
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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