The distance to the Orion Nebula

Menten, K. M.; Reid, M. J.; Forbrich, Jan; Brunthaler, A.

doi:10.1051/0004-6361:20078247

Cited by 766 publications

(803 citation statements)

References 32 publications

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“…It is located in the Orion Nebula Cluster, which has a distance of 414±7 pc [18] . It has a disk mass of 0.3 M and a bolometric luminosity of 400 L [19] .…”

Section: V883mentioning

confidence: 99%

“…The PA was again set to 32.4 • , while an inclination of 38.3 ± 1 • was determined from the ratio of the major and minor axes of the disk in the continuum image. We adopted a distance of 414 pc [18] while the source velocity (v src ) was set to 4.3 km s −1 based on the moment-1 map. The center of the disk was fixed to the center of the continuum image.…”

Section: V883mentioning

confidence: 99%

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Imaging the water snow-line during a protostellar outburst

Cieza

Casassus

Tobin

et al. 2016

Nature

198

246

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A snow-line is the region of a protoplanetary disk at which a major volatile, such as water or carbon monoxide, reaches its condensation temperature. Snowlines play a crucial role in disk evolution by promoting the rapid growth of icecovered grains 1−6 . Signatures of the carbon monoxide snow-line (at temperatures of around 20 kelvin) have recently been imaged with in the disks surrounding the pre-main-sequence stars TW Hydra 7−9 and HD163296 [3,10] , at distances of about 30 astronomical units (au) from the star. But the water snow-line of a protoplanetary disk (at temperatures of more than 100 kelvin) has not hitherto been seen, as it generally lies very close to the star (less than 5 au away for solartype stars 11 ). Water-ice is important because it regulates the efficiency of dust and planetesimal coagulation 5 , and the formation of comets, ice giants and the cores of gas giants 12 . Here we report ALMA images at 0.03-arcsec resolution (12 au) of the protoplanetary disk around V883 Ori, a protostar of 1.3 solar masses that is undergoing an outburst in luminosity arising from a temporary increase in the accretion rate 13 . We find an intensity break corresponding to an abrupt change in the optical depth at about 42 au, where the elevated disk temperature approaches the condensation point of water, from which we conclude that the outburst has moved the water snow-line. The spectral behaviour across the snow-line confirms recent model predictions 14 : dust fragmentation and the inhibition of grain growth at higher temperatures results in soaring grain number densities and optical depths. As most planetary systems are expected to experience outbursts caused by accretion during their formation [15,16] our results imply that highly dynamical water snow-lines must be considered when developing models of disk evolution and planet formation. V883Ori is an FU Ori object identified as such by [17] from followup spectroscopy of deeply embedded sources from the Infrared Astronomical Satellite (IRAS). It is located in the Orion Nebula Cluster, which has a distance of 414±7 pc [18] . It has a disk mass of 0.3 M and a bolometric luminosity of 400 L [19] . We have obtained 230 GHz/1.3 mm (band-6) observations of V883 Ori using the Atacama Large Millimeter/submillimeter Array (ALMA) in four different array configurations with baselines ranging from 14 m to 12.6 km, which were taken in ALMA Cycle-2 and Cycle-3. These new ALMA observations include continuum and the 12 CO, 13 CO, and C 18 O J = 2 -1 spectral lines. We use the C 18 O gas line to investigate the dynamics of the system at 0.2 (90 au) resolution and the continuum data to constrain the physical properties of the dust in the V883 Ori disk at 0.03 (12 au) resolution. In Figure 1 (top panel) we show our Cycle-3 continuum image at 0.03 resolution, the highest resolution ever obtained for a FU Ori object at millimeter wavelengths. We find that the V883 Ori disk has a two-region morphology, with a very bright inner disk (r ∼ 0.1 , 42 au) and a much more tenuous outer dis...

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“…It is located in the Orion Nebula Cluster, which has a distance of 414±7 pc [18] . It has a disk mass of 0.3 M and a bolometric luminosity of 400 L [19] .…”

Section: V883mentioning

confidence: 99%

Section: V883mentioning

confidence: 99%

Imaging the water snow-line during a protostellar outburst

Cieza

Casassus

Tobin

et al. 2016

Nature

198

246

View full text Add to dashboard Cite

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“…Orion-A GMC is located at a distance of 400 pc (Menten et al 2007;Sandstrom et al 2007;Hirota et al 2008) and is under strong influence of the FUV emission from the Trapezium cluster and NU Ori (Shimajiri et al 2011). Several photon dissociation regions (PDRs) have been identified from comparison of the distributions of the 8 μm, 1.1 mm, and 12 CO ( J = 1-0) line emission (Hollenbach & Tielens 1997;Shimajiri et al 2011Shimajiri et al , 2013.…”

Section: Comparison Between the L 1551 Molecular Cloud And The Orion-mentioning

confidence: 99%

The Intrinsic Abundance Ratio and X-Factor of Co Isotopologues in L 1551 Shielded From Fuv Photodissociation

Lin

Shimajiri

Hara

et al. 2016

ApJ

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We investigate the intrinsic abundance ratio of 13 CO to C 18 O and the X-factor in L 1551 using the Nobeyama Radio Observatory (NRO) 45 m telescope. L 1551 is chosen because it is relatively isolated in the Taurus molecular cloud shielded from FUV photons, providing an ideal environment for studying the target properties. Our observations cover~¢´¢ 40 40 with a resolution of~ 30 , which make up maps with the highest spatial dynamical range to date. We derive the X Xvalue on the sub-parsec scales in the range of ∼3-27 with a mean value of 8.0 ± 2.8. Comparing to the visual extinction map derived from the Herschel observations, we found that the abundance ratio reaches its maximum at low A V (i.e., A V ∼ 1-4 mag), and decreases to the typical solar system value of 5.5 inside L 1551 MC. The high X Xvalue at the boundary of the cloud is most likely due to the selective FUV photodissociation of C 18 O. This is in contrast with Orion-A where internal OB stars keep the abundance ratio at a high level, greater than ∼10. In addition, we explore the variation of the X-factor, because it is an uncertain, but widely used, quantity in extragalactic studies. We found that the X-factor µN H 1.0 2 , which is consistent with previous simulations. Excluding the high density region, the average X-factor is similar to the Milky Way average value.

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“…The blue contours in e) and f) represent the CH + 119.8 µm (≈9 resolution) and OH 84.6 µm (≈6 ) lines mapped by Herschel (Parikka et al 2017). few 10 4 times the mean interstellar radiation field. Because of its proximity (∼414 pc, Menten et al 2007) and nearly edge-on orientation, the Bar is a template to investigate the dynamics and chemistry in strongly FUV-irradiated gas (e.g., Pellegrini et al 2009;Cuadrado et al 2015;Goicoechea et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Spatially resolved images of reactive ions in the Orion Bar

Goicoechea

Cuadrado

Pety

et al. 2017

A&A

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We report high angular resolution (4.9 × 3.0 ) images of reactive ions SH + , HOC + , and SO + toward the Orion Bar photodissociation region (PDR). We used ALMA-ACA to map several rotational lines at 0.8 mm, complemented with multi-line observations obtained with the IRAM 30 m telescope. The SH + and HOC + emission is restricted to a narrow layer of 2 -to 10 -width (≈800 to 4000 AU depending on the assumed PDR geometry) that follows the vibrationally excited H * 2 emission. Both ions efficiently form very close to the H/H 2 transition zone, at a depth of A V 1 mag into the neutral cloud, where abundant C + , S + , and H * 2 coexist. SO + peaks slightly deeper into the cloud. The observed ions have low rotational temperatures (T rot ≈ 10−30 K T k ) and narrow line-widths (∼2−3 km s −1 ), a factor of 2 narrower that those of the lighter reactive ion CH + . This is consistent with the higher reactivity and faster radiative pumping rates of CH + compared to the heavier ions, which are driven relatively more quickly toward smaller velocity dispersion by elastic collisions and toward lower T rot by inelastic collisions. We estimate column densities and average physical conditions from an excitation model (n(H 2 ) ≈ 10 5 −10 6 cm −3 , n(e − ) ≈ 10 cm −3 , and T k ≈ 200 K). Regardless of the excitation details, SH + and HOC + clearly trace the most exposed layers of the UV-irradiated molecular cloud surface, whereas SO + arises from slightly more shielded layers.

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The distance to the Orion Nebula

Cited by 766 publications

References 32 publications

Imaging the water snow-line during a protostellar outburst

Imaging the water snow-line during a protostellar outburst

The Intrinsic Abundance Ratio and X-Factor of Co Isotopologues in L 1551 Shielded From Fuv Photodissociation

Spatially resolved images of reactive ions in the Orion Bar

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