Rosette globulettes and shells in the infrared

Mäkelä, Marko M.; Haikala, L. K.; Gahm, G. F.

doi:10.1051/0004-6361/201423440

Cited by 6 publications

(5 citation statements)

References 41 publications

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“…Gahm et al (2007) derived masses from extinction measures indicating that most objects have masses < 13 M J (Jupiter masses). Follow-up near-infrared (NIR) imaging and radio molecular line observations of the larger globulettes in the Rosette nebula, hereafter labelled RN, showed that these objects are dense and that the gas is molecular even close to the surface layers (Gahm et al 2013;hereafter called G13;Mäkelä et al 2014). Mass estimates derived from modelling the molecular line emission (based on the gas content) were found to be similar, but systematically higher compared to those derived from extinction (based on the dust content).…”

Section: Introductionmentioning

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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Section: Introductionmentioning

confidence: 99%

Radio observations of globulettes in the Carina nebula

Haikala

Gahm

Grenman

et al. 2017

A&A

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“…Some of these background clouds may be globules accelerated by the expansion of the Rosette Nebula H II region. With near-infrared imaging and mid-infrared and far-infrared data from Spitzer IRAC and Herschel PACS, Mäkelä et al (2014Mäkelä et al ( , 2017 investigated the physical properties and star formation activity of the globulettes and globules that lie in front of the Rosette Nebula and are associated with the C1 cloud. They found that the masses of globulettes are subsolar and the masses of globules are 9.5-11.6 M and that the globules RN A and RN E have velocities around 3 km s −1 which is similar to the velocity of cloud C1.…”

Section: Rmc Background Molecular Cloudsmentioning

confidence: 99%

“…The average velocity of the Rosette Nebula is 16.7 km s −1 (Dent et al 2009), therefore, it can be assumed that globules RN A and RN E have been accelerated by the Rosette Nebula H II region about 13.7 km s −1 toward the earth. Taking the results of Mäkelä et al (2014Mäkelä et al ( , 2017 as a reference on the masses of globules and the acceleration by the Rosette Nebula H II region, we consider the background molecular clouds that have masses less than 15 M and velocities less than 30.4 km s −1 as the possible globules blown out of the H II region on the far side. We recalculated the masses of the background molecular clouds with a fixed distance of 1.4 kpc rather than the kinematic distances derived from the Galactic rotation curve and it is found that 17 background molecular clouds satisfy the mass and velocity criterion.…”

Section: Rmc Background Molecular Cloudsmentioning

confidence: 99%

A Large-scale Survey of CO and Its Isotopologues toward the Rosette Molecular Cloud

Wang

Zhang

et al. 2018

ApJS

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Using the PMO-13.7m millimeter telescope at Delingha in China, we have conducted a large-scale simultaneous survey of 12 CO, 13 CO, and C 18 O J=1-0 emission toward the Rosette molecular cloud (RMC) region with a sky coverage of 3.5 • × 2.5 • . The majority of the emission in the region comes from the RMC complex with velocities lying in the range from -2 km s −1 to 20.5 km s −1 . Beyond this velocity range, 73 molecular clumps are identified with kinematic distances from 2.4 kpc to 11 kpc. Based on the spatial and velocity distribution, nine individual clouds, C1-C9, have been identified for the RMC complex. It appears that the C3 cloud is different from other clouds in the RMC complex in view of its characteristic velocity, excitation temperature, and velocity dispersion. Most of the young stellar clusters in the region are located in positions of both high column density and high excitation temperature. Seven new molecular filaments are discovered in the RMC complex. Evidence for cloud-cloud collision is found in the region of young stellar clusters REFL9 and PouF, showing that these young stellar clusters probably result from a cloud-cloud collision. The abundance ratios of 13 CO to C 18 O in the region have a mean value of 13.7 which is 2.5 times larger than the solar system value, showing that UV photons from the nearby OB clusters have strong influence on the chemistry of clouds in the RMC complex.

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“…Reipurth et al 2003;De Marco et al 2006;Gahm et al 2007) and even in the NIR (e.g. Mäkelä et al 2014), as they are seen as silhouettes against the bright nebular background emission. Despite their small sizes (4 to 20 ), the globulettes in the Rosette and Carina nebulae were well detected in 12 CO and 13 CO (3-2) and (2-1) lines at Atacama pathfinder experiment (APEX) (Gahm et al 2013;Haikala et al 2017).…”

Section: Introductionmentioning

confidence: 99%

ALMA detection of the dusty object silhouetted against the S0 galaxy NGC 3269 in the Antlia cluster

Haikala

Salinas

Richtler

et al. 2021

A&A

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Context. An intriguing silhouette of a small dust patch can be seen against the disk of the S0 galaxy NGC 3269 in the Antlia cluster in optical images. The images do not provide any clue as to whether the patch is a local Jupiter mass-scale cloudlet or a large extragalactic dust complex. Aims. We aim to resolve the nature of this object: is it a small Galactic cloudlet or an extragalactic dust complex? Methods. ALMA and APEX spectroscopy and Gemini GMOS long-slit spectroscopy were used to measure the velocity of the patch and the NGC 3269 disk radial velocity curve. Results. A weak 16±2.5 km s −1 wide 12 CO (2-1) T MB 19±2.5. mK line in a 2. 2 by 2. 12 beam associated with the object was detected with ALMA. The observed heliocentric velocity, V r,hel = 3878 ± 5.0km s −1 , immediately establishes the extragalactic nature of the object. The patch velocity is consistent with the velocity of the nucleus of NGC 3269, but not with the radial velocity of the NGC 3269 disk of the galaxy at its position. The ∼4 angular size of the patch corresponds to a linear size of ∼1 kpc at the galaxy's Hubble distance of 50.7 Mpc. The mass estimated from the 12 CO (2-1) emission is ∼1.4×10 6 (d/50.7 Mpc) 2 M , while the attenuation derived from the optical spectrum implies a dust mass of ∼2.6×10 4 (d/50.7 Mpc) 2 M. The derived attenuation ratio A B /(A B − A R) of 1.6±0.11 is substantially lower than the corresponding value for the mean Milky Way extinction curve for point sources (2.3). Conclusions. We established the extragalactic nature of the patch, but its origin remains elusive. One possibility is that the dust patch is left over from the removal of interstellar matter in NGC 3269 through the interaction with its neighbour, NGC 3268.

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Rosette globulettes and shells in the infrared

Cited by 6 publications

References 41 publications

Radio observations of globulettes in the Carina nebula

Radio observations of globulettes in the Carina nebula

A Large-scale Survey of CO and Its Isotopologues toward the Rosette Molecular Cloud

ALMA detection of the dusty object silhouetted against the S0 galaxy NGC 3269 in the Antlia cluster

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