Absolute proper motion of IRAS 00259+5625 with VERA: Indication of superbubble expansion motion

Sakai, Nobuyuki; Sato, M.; Motogi, Kazuhito; Nagayama, Tomonori; Shibata, Katsunori M.; Kanaguchi, Masahiro; Honma, Mareki

doi:10.1093/pasj/pst005

Cited by 16 publications

(6 citation statements)

References 43 publications

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“…estimated a kinematic distance of 2.5 kpc (which is the one adopted in this work), while Yun & Clemens (1994) obtained a CO velocity distance of 2.1 kpc using the rotation curve in Clemens (1985). The wa- ter maser proper motion suggests a distance of 2.6 +1.0 −0.6 kpc, consistent with previous estimates (Sakai et al 2014). compiled the 12-1300 µm flux of the continuum source, CB 3-mm, and derived a luminosity of 930 L and a gas mass of 72 M .…”

Section: Iras 00259+5625supporting

confidence: 89%

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

Fedriani¹,

Tan²,

Telkamp³

et al. 2022

Preprint

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We present ∼ 10 − 40 µm SOFIA-FORCAST images of 11 "isolated" protostars as part of the SOFIA Massive (SOMA) Star Formation Survey, with this morphological classification based on 37 µm imaging. We develop an automated method to define source aperture size based on the gradient of its background-subtracted enclosed flux and apply this to build spectral energy distributions (SEDs). We fit the SEDs with radiative transfer models, based on the Turbulent Core Accretion (TCA) theory, to estimate key protostellar properties. Here we release the sedcreator python package that carries out these methods. The SEDs are generally well-fit by the TCA models, from which we infer initial core masses M c ranging from 50 − 430 M , clump mass surface densities Σ cl ∼ 0.1 − 3 g cm −2 and current protostellar masses m * ∼ 2 − 40 M . From an uniform analysis of the 40 sources in the full SOMA survey to date, we find that massive protostars form across a wide range of clump mass surface density environments, placing constraints on theories that predict a minimum threshold Σ cl for massive star formation. However, the upper end of the m * − Σ cl distribution follows trends predicted by models of internal protostellar feedback that find greater star formation efficiency in higher Σ cl conditions. We also investigate protostellar FIR variability by comparison with IRAS data, finding no significant variation over a ∼40-year baseline.

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Section: Iras 00259+5625supporting

confidence: 89%

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

Fedriani¹,

Tan²,

Telkamp³

et al. 2022

Preprint

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“…• ) shows a large difference in distance -IRAS 00420+5530: 2.2 ± 0.05 kpc and NGC 281 W: 2.8 +0.26 −0.22 kpc (Sakai et al 2013). The size of the W4 superbubble is much larger than that of NGC 281, and so we can expect a much larger size for the W4 region.…”

Section: Total Mass Of Ic 1805mentioning

confidence: 85%

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

Sung

Bessell

Chun

et al. 2017

ApJS

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We present deep wide-field optical CCD photometry and mid-infrared Spitzer/IRAC and MIPS 24µm data for about 100,000 stars in the young open cluster IC 1805. The members of IC 1805 were selected from their location in the various color-color and color-magnitude diagrams, and the presence of Hα emission, mid-infrared excess emission, and X-ray emission. The reddening law toward IC 1805 is nearly normal (R V = 3.05 ± 0.06). However, the distance modulus of the cluster is estimated to be 11.9 ± 0.2 mag (d = 2.4 ± 0.2 kpc) from the reddening-free color-magnitude diagrams, which is larger than the distance to the nearby massive star-forming region W3(OH) measured from the radio VLBA astrometry. We also determined the age of IC 1805 (τ M ST O = 3.5 Myr). In addition, we critically compared the age and mass scale from two pre-main-sequence evolution models. The initial mass function with a Salpeter-type slope of Γ = -1.3 ± 0.2 was obtained and the total mass of IC 1805 was estimated to be about 2700 ± 200 M . Finally, we found our distance determination to be statistically consistent with the Tycho-Gaia Astrometric Solution Data Release 1, within the errors. The proper motion of the B-type stars shows an elongated distribution along the Galactic plane, which could be explained by some of the B-type stars being formed in small clouds dispersed by previous episodes of star formation or supernova explosions.

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“…Recently, Tremblin et al (2013) find that expanding HII regions or bubbles tend to induce steep density profiles in the cores at the bubble edges. Thus, the steep density profiles obtained in DR21-OH, AFGL 5142, CB3 (p ∼ 2) could have been produced by the expanding ionization fronts from the massive stars in these regions (Hunter et al 1995;Schneider et al 2011;Sakai et al 2013). A more detailed and uniform study of the turbulence mode in each core would be required to definitely assess the role of the different turbulence modes in setting the density structure of massive dense cores.…”

Section: Physical Processes Affecting the Density Structure Ofmentioning

confidence: 99%

Fragmentation of Massive Dense Cores Down to ≲ 1000 Au: Relation Between Fragmentation and Density Structure

Palau

Estalella

Girart

et al. 2014

ApJ

138

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In order to shed light on the main physical processes controlling fragmentation of massive dense cores, we present a uniform study of the density structure of 19 massive dense cores, selected to be at similar evolutionary stages, for which their relative fragmentation level was assessed in a previous work. We inferred the density structure of the 19 cores through a simultaneous fit of the radial intensity profiles at 450 and 850 µm (or 1.2 mm in two cases) and the Spectral Energy Distribution, assuming spherical symmetry and that the density and temperature of the cores decrease with radius following power-laws. Even though the estimated fragmentation level is strictly speaking a lower limit, its relative value is significant and several trends could be explored with our data. We find a weak (inverse) trend of fragmentation level and density power-law index, with steeper density profiles tending to show lower fragmentation, and vice versa. In addition, we find a trend of fragmentation increasing with density within a given radius, which arises from a combination of flat density profile and high central density and is consistent with Jeans fragmentation. We considered the effects of rotational-to-gravitational energy ratio, non-thermal velocity dispersion, and turbulence mode on the density structure of the cores, and found that compressive turbulence seems to yield higher central densities. Finally, a possible explanation for the origin of cores with concentrated density profiles, which are the cores showing no fragmentation, could be related with a strong magnetic field, consistent with the outcome of radiation magnetohydrodynamic simulations.

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Absolute proper motion of IRAS 00259+5625 with VERA: Indication of superbubble expansion motion

Cited by 16 publications

References 43 publications

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

Fragmentation of Massive Dense Cores Down to ≲ 1000 Au: Relation Between Fragmentation and Density Structure

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Absolute proper motion of IRAS 00259+5625 with VERA: Indication of superbubble expansion motion

Cited by 16 publications

References 43 publications

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* †

Fragmentation of Massive Dense Cores Down to ≲ 1000 Au: Relation Between Fragmentation and Density Structure

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Product

Resources

About

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†