870 <i>μ</i>m observations of evolved stars with LABOCA

Ladjal, D.; Justtanont, K.; Groenewegen, M. A. T.; Blommaert, J. A. D. L.; Waelkens, Christoffel; Barlow, M. J.

doi:10.1051/0004-6361/200913147

Cited by 36 publications

(47 citation statements)

References 84 publications

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“…3a) depending on the initial stellar mass and metallicity. These values are in agreement with subsequent submillimetre observations by Ladjal et al (2010) where dust masses of (0.01 − 2000) × 10 −5 M⊙ were measured in a sample of AGB stars, and are consistent with the recent AGB theoretical dust formation model of Ventura et al (2012) (Fig. 3a, red line).…”

Section: Dust From Lims -δ Limssupporting

confidence: 92%

The dust budget crisis in high-redshift submillimetre galaxies

Rowlands¹,

Gomez²,

Dunne³

et al. 2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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We apply a chemical evolution model to investigate the sources and evolution of dust in a sample of 26 high-redshift (z > 1) submillimetre galaxies (SMGs) from the literature, with complete photometry from ultraviolet to the submillimetre. We show that dust produced only by low-intermediate mass stars falls a factor 240 short of the observed dust masses of SMGs, the well-known 'dust-budget crisis'. Adding an extra source of dust from supernovae can account for the dust mass in 19 per cent of the SMG sample. Even after accounting for dust produced by supernovae the remaining deficit in the dust mass budget provides support for higher supernova yields, substantial grain growth in the interstellar medium or a top-heavy IMF. Including efficient destruction of dust by supernova shocks increases the tension between our model and observed SMG dust masses. The models which best reproduce the physical properties of SMGs have a rapid build-up of dust from both stellar and interstellar sources and minimal dust destruction. Alternatively, invoking a top-heavy IMF or significant changes in the dust grain properties can solve the dust budget crisis only if dust is produced by both low mass stars and supernovae and is not efficiently destroyed by supernova shocks.

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Section: Dust From Lims -δ Limssupporting

confidence: 92%

The dust budget crisis in high-redshift submillimetre galaxies

Rowlands¹,

Gomez²,

Dunne³

et al. 2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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“…This suggests that there is a problem with calibration for JCMT observations of this star. The object has been observed to be spherically symmetric on a large scale (Mauron & Huggins 2006) but with a small scale extension (e.g., Hofmann et al 2001;Inomata et al 2007;Ladjal et al 2010). In view of this, we take the simplest approach of fitting the HIFI and ground-based lines with a constant mass loss rate.…”

Section: Wx Psc (Irc+10011)mentioning

confidence: 99%

OH/IR stars and their superwinds as observed by theHerschelSpace Observatory

Justtanont

Teyssier

Barlow

et al. 2013

A&A

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Aims. In order to study the history of mass loss in extreme OH/IR stars, we observed a number of these objects using CO as a tracer of the density and temperature structure of their circumstellar envelopes. Methods. Combining CO observations from the Herschel Space Observatory with those from the ground, we trace mass loss rates as a function of radius in five extreme OH/IR stars. Using radiative transfer modelling, we modelled the dusty envelope as well as the CO emission. The high-rotational transitions of CO indicate that they originate in a dense superwind region close to the star while the lower transitions tend to come from a more tenuous outer wind which is a result of the mass loss since the early AGB phase.Results. The models of the circumstellar envelopes around these stars suggest that they have entered a superwind phase in the past 200-500 years. The low 18 O/ 17 O (∼0.1 compared to the solar abundance ratio of ∼5) and 12 C/ 13 C (3-30 cf. the solar value of 89) ratios derived from our study support the idea that these objects have undergone hot-bottom burning and hence that they are massive M ≥ 5 M AGB stars.

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“…Ladjal et al 2010). The infrared SEDs of evolved stars can be quite similar to those of YSOs, and thus the nature of objects selected by criteria based on infrared excess alone is not immediately clear and can lead to ambiguities (e.g.…”

Section: Evolved Starsmentioning

confidence: 99%

Herschelfar-infrared observations of the Carina Nebula complex

Gaczkowski

Preibisch

Ratzka

et al. 2012

A&A

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Context. The Carina Nebula represents one of the largest and most active star forming regions known in our Galaxy. It contains numerous very massive (M > ∼ 40 M ) stars that strongly affect the surrounding clouds by their ionizing radiation and stellar winds. Aims. Our recently obtained Herschel PACS and SPIRE far-infrared maps cover the full area (≈8.7 deg 2 ) of the Carina Nebula complex (CNC) and reveal the population of deeply embedded young stellar objects (YSOs), most of which are not yet visible in the mid-or near-infrared. Methods. We study the properties of the 642 objects that are independently detected as point-like sources in at least two of the five Herschel bands. For those objects that can be identified with apparently single Spitzer counterparts, we use radiative transfer models to derive information about the basic stellar and circumstellar parameters. Results. We find that about 75% of the Herschel-detected YSOs are Class 0 protostars. The luminosities of the Herschel-detected YSOs with SED fits are restricted to values of ≤5400 L , their masses (estimated from the radiative transfer modeling) range from ≈1 M to ≈10 M . Taking the observational limits into account and extrapolating the observed number of Herschel-detected protostars over the stellar initial mass function suggest that the star formation rate of the CNC is ∼0.017 M /year. The spatial distribution of the Herschel YSO candidates is highly inhomogeneous and does not follow the distribution of cloud mass. Rather, most Herschel YSO candidates are found at the irradiated edges of clouds and pillars. The far-infrared fluxes of the famous object η Car are about a factor of two lower than expected from observations with the Infrared Space Observatory obtained 15 years ago; this difference may be a consequence of dynamical changes in the circumstellar dust in the Homunculus Nebula around η Car. Conclusions. The currently ongoing star formation process forms only low-mass and intermediate-mass stars, but no massive (M > ∼ 20 M ) stars. The characteristic spatial configuration of the YSOs provides support to the picture that the formation of this latest stellar generation is triggered by the advancing ionization fronts.

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870 μm observations of evolved stars with LABOCA

Cited by 36 publications

References 84 publications

The dust budget crisis in high-redshift submillimetre galaxies

The dust budget crisis in high-redshift submillimetre galaxies

OH/IR stars and their superwinds as observed by theHerschelSpace Observatory

Herschelfar-infrared observations of the Carina Nebula complex

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