Protoplanetary Disks in the Hostile Environment of Carina

Mesa‐Delgado, A.; Zapata, Luis A.; Henney, W. J.; Puzia, Thomas H.; Tsamis, Y. G.

doi:10.3847/2041-8205/825/1/l16

Cited by 36 publications

(37 citation statements)

References 45 publications

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“…They concentrate on those indices that are best reproduced by the Bruzual & Charlot (2003) models with a fixed IMF 5 . A recent mass-metallicity relation measurement by González Delgado et al (2014) with the CALIFA integral field spectrograph for a sample of 300 galaxies, ranging from ellipticals to late-type spirals, agrees well with the SDSS measurements by Gallazzi et al (2005). At a given mass, the scatter in the metallicity is expected to be mostly intrinsic, rather than due to measurement uncertainties (see fig.…”

Section: The Vazdekis Imfsupporting

confidence: 68%

Implications of a variable IMF for the interpretation of observations of galaxy populations

Clauwens

Schaye

Franx

2016

Mon. Not. R. Astron. Soc.

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We investigate the effect of a metallicity-dependent stellar initial mass function (IMF), as deduced observationally by Martín-Navarro et al. (2015c), on the inferred stellar masses and star formation rates (SFRs) of a representative sample of 186,886 SDSS galaxies. Relative to a Chabrier IMF, for which we show the implied masses to be close to minimal, the inferred masses increase in both the low-and high-metallicity regimes due to the addition of stellar remnants and dwarf stars, respectively. The resulting galaxy stellar mass function (GSMF) shifts toward higher masses by 0.5 dex, without affecting the high-mass slope (and thus the need for effective quenching). The implied low-redshift SFR density increases by an order of magnitude. However, these results depend strongly on the assumed IMF parametrisation, which is not directly constrained by the observations. Varying the low-end IMF slope instead of the highend IMF slope, while maintaining the same dwarf-to-giant ratio, results in a much more modest GSMF shift of 0.2 dex and a 10 per cent increase in the SFR density relative to the Chabrier IMF. A bottom-heavy IMF during the late, metal-rich evolutionary stage of a galaxy would help explain the rapid quenching and the bimodality in the galaxy population by on the one hand making galaxies less quenched (due to the continued formation of dwarf stars) and on the other hand reducing the gas consumption timescale. We conclude that the implications of the observational evidence for a variable IMF could vary from absolutely dramatic to mild but significant.

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Section: The Vazdekis Imfsupporting

confidence: 68%

Implications of a variable IMF for the interpretation of observations of galaxy populations

Clauwens

Schaye

Franx

2016

Mon. Not. R. Astron. Soc.

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“…This object was observed before in different molecular transitions by Sahai et al (2012), who recognized an IR star within the globule as the driving source of the outflow. The embedded star is of intermediate mass according to Mesa-Delgado et al (2016) and Reiter et al (2016). In the following we refer to all objects as globulettes.…”

Section: Selected Objectsmentioning

confidence: 99%

Radio observations of globulettes in the Carina nebula

Haikala

Gahm

Grenman

et al. 2017

A&A

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Context. The Carina nebula hosts a large number of globulettes. An optical study of these tiny molecular clouds shows that the majority are of planetary mass, but there are also those with masses of several tens up to a few hundred Jupiter masses. Aims. We seek to search for, and hopefully detect, molecular line emission from some of the more massive objects; in case of successful detection we aim to map their motion in the Carina nebula complex and derive certain physical properties. Methods. We carried out radio observations of molecular line emission in 12 CO and 13 CO (2-1) and (3-2) of 12 globulettes in addition to positions in adjacent shell structures using APEX. Results. All selected objects were detected with radial velocities shifted relative to the emission from related shell structures and background molecular clouds. Globulettes along the western part of an extended dust shell show a small spread in velocity with small velocity shifts relative to the shell. This system of globulettes and shell structures in the foreground of the bright nebulosity surrounding the cluster Trumpler 14 is expanding with a few km s −1 relative to the cluster. A couple of isolated globulettes in the area move at similar speed. Compared to similar studies of the molecular line emission from globulettes in the Rosette nebula, we find that the integrated line intensity ratios and line widths are very different. The results show that the Carina objects have a different density/temperature structure than those in the Rosette nebula. In comparison the apparent size of the Carina globulettes is smaller, owing to the larger distance, and the corresponding beam filling factors are small. For this reason we were unable to carry out a more detailed modelling of the structure of the Carina objects in the way as performed for the Rosette objects. Conclusions. The Carina globulettes observed are compact and denser than objects of similar mass in the Rosette nebula. The distribution and velocities of these globulettes suggest that they have originated from eroding shells and elephant trunks. Some globulettes in the Trumpler 14 region are quite isolated and located far from any shell structures. These objects move at a similar speed as the globulettes along the shell, suggesting that they once formed from cloud fragments related to the same foreground shell.

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“…Therefore, taking a mass of 0.1 M for the pillar HH 901, we obtain that the pillar will be photo-evaporated in around 10 5 years. This timescale is shorter to that estimated, for example, for the massive EGG or globulette 105-600 (Mesa-Delgado et al 2016) of about 10 6 years. However, the 105-600 globulette is farther away from the Tr 14 massive cluster (17 pc), and is more massive (0.1 to 0.3 M ), which explains the large difference.…”

Section: N2d+(3−2)mentioning

confidence: 60%

“…Very recently, Mesa-Delgado et al (2016) using ALMA (Atacama Large Millimeter/Submillimeter Array) Band 6 Long Baseline continuum observations reported the first direct imaging of protoplanetary disks in the star-forming region of Carina and studied their possible external strong photo-evaporation. They detected a few protoplanetary disks (CN104-593 and CN105-600) in the highly obscured globules within the Carina Nebula and found no signs of disks near to the massive clusters Tr 14 and Tr 16.…”

Section: Introductionmentioning

confidence: 99%

ALMA Observations of the Extraordinary Carina Pillars: HH 901/902

Cortes-Rangel¹,

Zapata²,

Toalá³

et al. 2020

Self Cite

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We present Atacama Large Millimeter/Submillimeter Array (ALMA) 1.3 mm continuum and C 18 O(2−1), N 2 D + (3−2), 13 CS(5−4), and 12 CO(2−1) line sensitive and high angular resolution (∼0.3 ) observations of the famous carina pillars and protostellar objects HH 901/902. Our observations reveal for the first time, the bipolar CO outflows and the dusty disks (plus envelopes) that are energizing the extended and irradiated HH objects far from the pillars. We find that the masses of the disks+envelopes are about 0.1 M and of the bipolar outflows are between 10 −3 -10 −4 M , which suggests that they could be low-or maybe intermediate-mass protostars. Moreover, we suggest that these young low-mass stars are likely embedded Class 0/I protostars with high-accretion rates. We also show the kinematics of the gas in the pillars together with their respective gas masses (0.1 -0.2 M ). We estimate that the pillars will be photo-evaporated in 10 4 to 10 5 years by the massive and luminous stars located in the Trumpler 14 cluster. Finally, given the short photo-evaporated timescales and that the protostars in these pillars are still very embedded, we suggest that the disks inside of the pillars will be quickly affected by the radiation of the massive stars, forming proplyds, like those observed in Orion.

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Protoplanetary Disks in the Hostile Environment of Carina

Cited by 36 publications

References 45 publications

Implications of a variable IMF for the interpretation of observations of galaxy populations

Implications of a variable IMF for the interpretation of observations of galaxy populations

Radio observations of globulettes in the Carina nebula

ALMA Observations of the Extraordinary Carina Pillars: HH 901/902

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