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46 results on '"Rigby A.J."'

1. Towards the first mean pressure profile estimate with the NIKA2 Sunyaev-Zeldovich Large Program

Author

Hanser C., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Ferragamo A., Gomez A., Goupy J., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Paliwal A., Payerne C., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., and Tucker C.

Subjects
Physics, QC1-999
Abstract

High-resolution mapping of the hot gas in galaxy clusters is a key tool for cluster-based cosmological analyses. Taking advantage of the NIKA2 millimeter camera operated at the IRAM 30-m telescope, the NIKA2 SZ Large Program seeks to get a high-resolution follow-up of 38 galaxy clusters covering a wide mass range at intermediate to high redshift. The measured SZ fluxes will be essential to calibrate the SZ scaling relation and the galaxy clusters mean pressure profile, needed for the cosmological exploitation of SZ surveys. We present in this study a method to infer a mean pressure profile from cluster observations. We have designed a pipeline encompassing the map-making and the thermodynamical properties estimates from maps. We then combine all the individual fits, propagating the uncertainties on integrated quantities, such as R500 or P500, and the intrinsic scatter coming from the deviation to the standard self-similar model. We validate the proposed method on realistic LPSZ-like cluster simulations.

Published
2024
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2. Exploring the interstellar medium of NGC 891 at millimeter wavelengths using the NIKA2 camera

Author

Katsioli S., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Baes M., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., Clark C.J.R., De Looze I., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Galametz M., Galliano F., Gomez A., Goupy J., Hanser C., Hughes A., Kéruzoré F., Kramer C., Jones A.P., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Nersesian A., Pantoni L., Paradis D., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Smith M.W.L., Tedros J., Tabatabaei F., Tucker C., Xilouris E.M., Ysard N., and Zylka R.

Subjects
Physics, QC1-999
Abstract

In the framework of the IMEGIN Large Program, we used the NIKA2 camera on the IRAM 30-m telescope to observe the edge-on galaxy NGC 891 at 1.15 mm and 2 mm and at a FWHM of 11.1” and 17.6”, respectively. Multiwavelength data enriched with the new NIKA2 observations fitted by the HerBIE SED code (coupled with the THEMIS dust model) were used to constrain the physical properties of the ISM. Emission originating from the diffuse dust disk is detected at all wavelengths from mid-IR to mm. while mid-lR observations reveal warm dust emission from compact H II regions. Indications of mm excess emission have also been found in the outer parts of the galactic disk. Furthermore, our SED fitting analysis constrained the mass fraction of the small (< 15 Å) dust grains. We found that small grains constitute 9.5% of the total dust mass in the galactic plane, but this fraction increases up to ~ 20% at large distances (|z| > 3 kpc) from the galactic plane.

Published
2024
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3. NIKA2 observations of starless cores in Taurus and Perseus

Author

Kramer C., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Caselli P., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Fuente A., Gomez A., Goupy J., Hanser C., Katsioli S., Kéruzoré F., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J. F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Navarro-Almaida D., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Tucker C., and Zylka R.

Subjects
Physics, QC1-999
Abstract

Dusty starless cores play an important role in regulating the initial phases of the formation of stars and planets. In their interiors, dust grains coagulate and ice mantles form, thereby changing the millimeter emissivities and hence the ability to cool. We mapped four regions with more than a dozen cores in the nearby Galactic filaments of Taurus and Perseus using the NIKA2 camera at the IRAM 30-meter telescope. Combining the 1mm to 2mm flux ratio maps with dust temperature maps from Herschel allowed to create maps of the dust emissivity index β1,2 at resolutions of 2430 and 5600 a.u. in Taurus and Perseus, respectively. Here, we study the variation with total column densities and environment. β1,2 values at the core centers (Av =12 – 19 mag) vary significantly between ~ 1.1 and 2.3. Several cores show a strong rise of β1,2 from the outskirts at ~ 4 mag to the peaks of optical extinctions, consistent with the predictions of grain models and the gradual build-up of ice mantles on coagulated grains in the dense interiors of starless cores.

Published
2024
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4. Constraining millimeter dust emission in nearby galaxies with NIKA2: The case of NGC2146 and NGC2976

Author

Ejlali G., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Baes M., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Galliano F., Gomez A., Goupy J., Jones A.P., Hanser C., Hughes A., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S. C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Nersesian A., Pantoni L., Paradis D., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Smith M.W.S.L., Tabatabaei F.S., Tedros J., Tucker C., Xilouris E.M., and Zylka R.

Subjects
Physics, QC1-999
Abstract

This study presents the first millimeter continuum mapping observations of two nearby galaxies, the starburst spiral galaxy NGC2146 and the dwarf galaxy NGC2976, at 1.15 mm and 2 mm using the NIKA2 camera on the IRAM 30m telescope, as part of the Guaranteed Time Large Project IMEGIN. These observations provide robust resolved information about the physical properties of dust in nearby galaxies by constraining their FIR-radio SED in the millimeter domain. After subtracting the contribution from the CO line emission, the SEDs are modeled spatially using a Bayesian approach. Maps of dust mass surface density, temperature, emissivity index, and thermal radio component of the galaxies are presented, allowing for a study of the relations between the dust properties and star formation activity (using observations at 24μm as a tracer). We report that dust temperature is correlated with star formation rate in both galaxies. The effect of star formation activity on dust temperature is stronger in NGC2976, an indication of the thinner interstellar medium of dwarf galaxies. Moreover, an anti-correlation trend is reported between the dust emissivity index and temperature in both galaxies.

Published
2024
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5. NIKA2 observations of dust grain evolution from star-forming filament to T-Tauri disk: Preliminary results from NIKA2 observations of the Taurus B211/B213 filament

Author

Nguyen-Luong Q., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Gomez A., Goupy J., Hanser C., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J. F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Tucker C., Zylka R., Bacmann A., Duong-Tuan A., Peretto N., and Rigby A.

Subjects
Physics, QC1-999
Abstract

To understand the evolution of dust properties in molecular clouds in the course of the star formation process, we constrain the changes in the dust emissivity index from star-forming filaments to prestellar and protostellar cores to T Tauri stars. Using the NIKA2 continuum camera on the IRAM 30 m telescope. we observed the Taurus B211/B2I3 filament at 1.2 mm and 2 mm with unprecedented sensitivity and used the resulting maps to derive the dust emissivity index β. Our sample of 105 objects detected in the β map of the B211/B213 filament indicates that, overal. β decreases from filament and prestellar cores (β ~ 2 ± 0.5) to protostellar cores (β ~ 1.2 ± 0.2) to T-Tauri protoplanetary disk (β < I). The averaged dust emissivity index β across the B211/B2I3 filament exhibits a flat (β ~ 2 ± 0.3) profile. This may imply that dust grain sizes are rather homogeneous in the filament, start to grow significantly in size only after the onset of the gravitational contraction/collapse of prestellar cores to protostars, reaching big sizes in T Tauri protoplanetary disks. This evolution from the parent filament to T-Tauri disks happens on a timescale of about 1-2 Myr.

Published
2024
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6. IAS/CEA Evolution of Dust in Nearby Galaxies (ICED): The spatially-resolved dust properties of NGC4254

Author

Pantoni L., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Baes M., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Galliano F., Gomez A., Goupy J., Jones A.P., Hanser C., Hughes A., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S. C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Nersesian A., Paradis D., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Smith M.W.S.L., Tabatabaei F.S., Tedros J., Tucker C., Xilouris E.M., and Zylka R.

Subjects
Physics, QC1-999
Abstract

We present the first preliminary results of the project ICED, focusing on the face-on galaxy NGC4254. We use the millimetre maps observed with NIKA2 at lRAM-30m. as part of the IMEGIN Guaranteed Time Large Program. and of a wide collection of ancillary data (multi-wavelength photometry and gas phase spectral lines) that are publicly available. We derive the global and local properties of interstellar dust grains through infrared-to-radio spectral energy distribution fitting, using the hierarchical Bayesian code HerBIE. which includes the grain properties of the state-of-the-art dust model. THEMIS. Our method allows us to get the following dust parameters: dust mass, average interstellar radiation field, and fraction of small grains. Also, it is effective in retrieving the intrinsic correlations between dust parameters and interstellar medium properties. We find an evident anti-correlation between the interstellar radiation field and the fraction of small grains in the centre of NGC4254. meaning that, at strong radiation field intensities, very small amorphous carbon grains are efficiently destroyed by the ultra-violet photons coming from newly formed stars, through photo-desorption and sublimation. We observe a flattening of the anti-correlation at larger radial distances, which may be driven by the steep metallicity gradient measured in NGC4254.

Published
2024
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7. Stellar and dust emission profiles of IMEGIN galaxies

Author

Nersesian A., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Baes M., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Gomez A., Goupy J., Hanser C., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J. F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Pantoni L., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Tucker C., Xilouris E.M., and Zylka R.

Subjects
Physics, QC1-999
Abstract

We present a morphological analysis of a set of spiral galaxies from the NIKA2 Guaranteed Time Large Program, IMEGIN. We have fitted a single Sérsic model on a set of broadband images, from ultra-violet (UV) to millimeter (mm) wavelengths, using the modelling code Statmorph. With the recently acquired NIKA2 1.15- and 2-mm observations, it is possible to extend such a morphological analysis to the mm regime and investigate the two-dimensional (2D) distribution (exponential, Gaussian) of the very cold dust (

Published
2024
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8. Systematic effects on the upcoming NIKA2 LPSZ scaling relation

Author

Moyer-Anin A., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Gomez A., Goupy J., Hanser C., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., and Tucker C.

Subjects
Physics, QC1-999
Abstract

In cluster cosmology, cluster masses are the main parameter of interest. They are needed to constrain cosmological parameters through the cluster number count. As the mass is not an observable, a scaling relation is needed to link cluster masses to the integrated Compton parameters Y, i.e. the Sunyaev-Zeldovich observable (SZ). Planck cosmological results obtained with cluster number counts are based on a scaling relation measured with clusters at low redshift (z

Published
2024
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9. Exploring the millimetre emission in nearby galaxies: Analysis of the edge-on galaxy NGC 891

Author

Katsioli S., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Looze I., De Petris M., Désert F.-X., Doyle S., Driessen E.F. C., Ejlali G., Galametz M., Galliano F., Gomez A., Goupy J., Jones A.P., Hughes A., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Nersesian A., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Smith M. W. L., Tabatabaei F., Tucker C., Xilouris E. M., and Zylka R.

Subjects
Physics, QC1-999
Abstract

New observations of the edge-on galaxy NGC 891, at 1.15 and 2mm obtained with the IRAM 30-m telescope and the NIKA2 camera, within the framework of the IMEGIN (Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA2) Large Program, are presented in this work. By using multiwavelength maps (from the mid-IR to the cm wavelengths) we perform SED fitting in order to extract the physical properties of the galaxy on both global and local (~kpc) scales. For the interpretation of the observations we make use of a state-of-the-art SED fitting code, HerBIE (HiERarchical Bayesian Inference for dust Emission). The observations indicate a galaxy morphology, at mm wavelengths, similar to that of the cold dust emission traced by submm observations and to that of the molecular gas. The contribution of the radio emission at the NIKA2 bands is very small (negligible at 1.15 mm and ~ 10% at 2 mm) while it dominates the total energy budget at longer wavelengths (beyond 5 mm). On local scales, the distribution of the free-free emission resembles that of the dust thermal emission while the distribution of the synchrotron emission shows a deficiency along the major axis of the disc of the galaxy.

Published
2022
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10. Searching for high-z DSFGs with NIKA2 and NOEMA

Author

Bing L., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Beelen A., Benoît A., Berta S., Béthermin M., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Neri R., Omont A., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Zylka R.

Subjects
Physics, QC1-999
Abstract

As the possible progenitors of passive galaxies at z=2-3, dusty starforming galaxies (DSFGs) at z>4 provide a unique perspective to study the formation, assembly, and early quenching of massive galaxies in the early Universe. The extreme obscuration in optical-IR makes (sub)mm spectral scans the most universal and unbiased way to confirm/exclude the high-z nature of candidate dusty star-forming galaxies. We present here the status of the NIKA2 Cosmological Legacy Survey (N2CLS), which is the deepest wide-area singledish survey in the millimeter searching for high-z DSFGs. We also introduce a joint-analysis method to effciently search for the spectroscopic redshift of high-z DSFGs with noisy spectra and photometric data and present its success in identifying the redshift of DSFGs found in NIKA2 science verification data.

Published
2022
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11. Galactic Star Formation with NIKA2 (GASTON): Evidence of mass accretion onto dense clumps

Author

Rigby A.J., Adam R., Ade P., Ajeddig H., Anderson M., André P., Artis E., Aussel H., Bacmann A., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Bracco A., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., García P., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Peretto N., Perotto L., Pisano G., Ponthieu N., Revéret V., Ristorcelli I., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., Watkins E.J., and Zylka R.

Subjects
Physics, QC1-999
Abstract

High-mass stars (m* ≳ 8 M⊙) play a crucial role in the evolution of galaxies, and so it is imperative that we understand how they are formed. We have used the New IRAM KIDs Array 2 (NIKA2) camera on the Institut de Radio Astronomie Millimétrique (IRAM) 30-m telescope to conduct high-sensitivity continuum mapping of ~ 2 deg2 of the Galactic plane (GP) as part of the Galactic Star Formation with NIKA2 (GASTON) large program. We have identified a total of 1467 clumps within our deep 1.15 mm continuum maps and, by using overlapping continuum, molecular line, and maser parallax data, we have determined their distances and physical properties. By placing them upon an approximate evolutionary sequence based upon 8 μm Spitzer imaging, we find evidence that the most massive dense clumps accrete material from their surrounding environment during their early evolution, before dispersing as star formation advances, supporting clump-fed models of high-mass star formation.

Published
2022
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12. Probing the role of magnetic fields in star-forming filaments: NIKA2-Pol commissioning results toward OMC-1

Author

Ajeddig H., Adam R., Ade P., André P., Artis E., Aussel H., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., Zylka R., and Shimajiri Y.

Subjects
Physics, QC1-999
Abstract

Dust polarization observations are a powerful, practical tool to probe the geometry (and to some extent, the strength) of magnetic fields in starforming regions. In particular, Planck polarization data have revealed the importance of magnetic fields on large scales in molecular clouds. However, due to insufficient resolution, Planck observations are unable to constrain the B-field geometry on prestellar and protostellar scales. The high angular resolution of 11.7 arcsec provided by NIKA2-Pol 1.15 mm polarimetric imaging, corresponding to 0.02 pc at the distance of the Orion molecular cloud (OMC), makes it possible to advance our understanding of the B-field morphology in star-forming filaments and dense cores (IRAM 30m large program B-FUN). The commissioning of the NIKA2-Pol instrument has led to several challenging issues, in particular, the instrumental polarization or intensity-to-polarization “leakage” effect. In the present paper, we illustrate how this effect can be corrected for, leading to reliable exploitable data in a structured, extended source such as OMC-1. We present a statistical comparison between NIKA2-Pol and SCUBA2-Pol2 results in the OMC-1 region. We also present tentative evidence of local pinching of the B-field lines near Orion-KL, in the form of a new small-scale hourglass pattern, in addition to the larger-scale hourglass already seen by other instruments such as Pol2.

Published
2022
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13. Dust Emission in Galaxies at Millimeter Wavelengths: Cooling of star forming regions in NGC6946

Author

Ejlali G., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., de Looze I., De Petris M., Désert F.-X., Doyle S., Driessen E.F. C., Galametz M., Galliano F., Gomez A., Goupy J., Jones A.P., Hughes A., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Nersesian A., Perotto L., Pisano G., Ponthieu N., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Smith M. W. S. L., Tabatabaei F. S., Tucker C., Xilouris E.M., and Zylka R.

Subjects
Physics, QC1-999
Abstract

Interstellar dust plays an important role in the formation of molecular gas and the heating and cooling of the interstellar medium. The spatial distribution of the mm-wavelength dust emission from galaxies is largely unexplored. The NIKA2 Guaranteed Time Project IMEGIN (Interpreting the Millimeter Emission of Galaxies with IRAM and NIKA2) has recently mapped the mm emission in the grand design spiral galaxy NGC6946. By subtracting the contributions from the free-free, synchrotron, and CO line emission, we map the distribution of the pure dust emission at 1:15mm and 2mm. Separating the arm/interarm regions, we find a dominant 2mm emission from interarms indicating the significant role of the general interstellar radiation field in heating the cold dust. Finally, we present maps of the dust mass, temperature, and emissivity index using the Bayesian MCMC modeling of the spectral energy distribution in NGC6946.

Published
2022
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14. NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts

Author

Bing, L, Béthermin, M, Lagache, G, Adam, R, Ade, P, Ajeddig, H, André, P, Artis, E, Aussel, H, Beelen, A, Benoît, A, Berta, S, Billot, N, Bourrion, O, Calvo, M, Catalano, A, de Petris, M, Désert, F.-X, Doyle, S, Driessen, E.F.C, Elbaz, D, Gkogkou, A, Gomez, A, Goupy, J, Hanser, C, Kéruzoré, F, Kramer, C, Ladjelate, B, Liu, D, Leclercq, S, Lestrade, J.-F, Lustig, P, Macías-Pérez, J.F, Maury, A, Mauskopf, P, Mayet, F, Monfardini, A, Muñoz-Echeverría, M, Perotto, L, Pisano, G, Ponthieu, N, Revéret, V, Rigby, A.J, Ritacco, A, Romero, C, Roussel, H, Ruppin, F, Schuster, K, Sievers, A, Tucker, C, Zylka, R, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Aims. Deep millimeter surveys are necessary to probe the dust-obscured galaxies at high redshift. We conducted a large observing program at 1.2 and 2 mm with the NIKA2 camera installed on the IRAM 30-meter telescope. This NIKA2 Cosmological Legacy Survey (N2CLS) covers two emblematic fields: GOODS-N and COSMOS. We introduce the N2CLS survey and present new 1.2 and 2 mm number count measurements based on the tiered N2CLS observations from October 2017 to May 2021. Methods. We develop an end-to-end simulation that combines an input sky model with the instrument noise and data reduction pipeline artifacts. This simulation is used to compute the sample purity, flux boosting, pipeline transfer function, completeness, and effective area of the survey. We used the 117 deg$^2$ SIDES simulations as the sky model, which include the galaxy clustering. Our formalism allows us to correct the source number counts to obtain galaxy number counts, the difference between the two being due to resolution effects caused by the blending of several galaxies inside the large beam of single-dish instruments. Results. The N2CLS-May2021 survey reaches an average 1-$\sigma$ noise level of 0.17 and 0.048 mJy on GOODS-N over 159 arcmin$^2$, and 0.46 and 0.14 mJy on COSMOS over 1010 arcmin$^2$, at 1.2 and 2 mm, respectively. For a purity threshold of 80%, we detect 120 and 67 sources in GOODS-N and 195 and 76 sources in COSMOS, at 1.2 and 2 mm, respectively. Our measurement connects the bright single-dish to the deep interferometric number counts. After correcting for resolution effects, our results reconcile the single-dish and interferometric number counts and are further accurately compared with model predictions., Comment: Accepted by A&A. 23 pages, 12 figures

Published
2023
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15. The SEDIGISM survey: Molecular cloud morphology. II: Integrated source properties

Author

Neralwar, K.R., Colombo, D., Duarte-Cabral, A., Urquhart, J.S., Mattern, M., Wyrowski, F., Menten, K.M., Barnes, P., Sánchez-Monge, Á., Rigby, A.J., Mazumdar, P., Eden, D., Csengeri, T., Dobbs, C. L., Veena, V. S., Neupane, S., Henning, T., Schuller, F., Leurini, S., Wienen, M., Yang, A. Y., Ragan, S.E., Medina, S., Nguyen-Luong, Q., Neralwar, K.R., Colombo, D., Duarte-Cabral, A., Urquhart, J.S., Mattern, M., Wyrowski, F., Menten, K.M., Barnes, P., Sánchez-Monge, Á., Rigby, A.J., Mazumdar, P., Eden, D., Csengeri, T., Dobbs, C. L., Veena, V. S., Neupane, S., Henning, T., Schuller, F., Leurini, S., Wienen, M., Yang, A. Y., Ragan, S.E., Medina, S., and Nguyen-Luong, Q.

Abstract

The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey has produced high (spatial and spectral) resolution 13CO (2–1) maps of the Milky Way. It has allowed us to investigate the molecular interstellar medium in the inner Galaxy at an unprecedented level of detail and characterise it into molecular clouds. In a previous paper, we have classified the SEDIGISM clouds into four morphologies. However, how the properties of the clouds vary for these four morphologies is not well understood. Here, we use the morphological classification of SEDIGISM clouds to find connections between the cloud morphologies, their integrated properties, and their location on scaling relation diagrams. We observe that ring-like clouds show the most peculiar properties, having, on average, higher masses, sizes, aspect ratios and velocity dispersions compared to other morphologies. We speculate that this is related to the physical mechanisms that regulate their formation and evolution, for example, turbulence from stellar feedback can often results in the creation of bubble-like structures. We also see a trend of morphology with virial parameter whereby ring-like, elongated, clumpy and concentrated clouds have virial parameters in a decreasing order. Our findings provide a foundation for a better understanding of the molecular cloud behaviour based on their measurable properties.

Published
2022

16. The SEDIGISM survey: Molecular cloud morphology. I. Classification and star formation

Author

Neralwar, K.R., Colombo, D., Duarte-Cabral, A., Urquhart, J.S., Mattern, M., Wyrowski, F., Menten, K.M., Barnes, P., Sánchez-Monge, Á., Beuther, H., Rigby, A.J., Mazumdar, P., Eden, D., Csengeri, T., Dobbs, C. L., Veena, V. S., Neupane, S., Henning, T., Schuller, F., Leurini, S., Wienen, M., Yang, A. Y., Ragan, S.E., Medina, S., Nguyen-Luong, Q., Neralwar, K.R., Colombo, D., Duarte-Cabral, A., Urquhart, J.S., Mattern, M., Wyrowski, F., Menten, K.M., Barnes, P., Sánchez-Monge, Á., Beuther, H., Rigby, A.J., Mazumdar, P., Eden, D., Csengeri, T., Dobbs, C. L., Veena, V. S., Neupane, S., Henning, T., Schuller, F., Leurini, S., Wienen, M., Yang, A. Y., Ragan, S.E., Medina, S., and Nguyen-Luong, Q.

Abstract

We present one of the very first extensive classifications of a large sample of molecular clouds based on their morphology. This is achieved using a recently published catalogue of 10663 clouds obtained from the first data release of the SEDIGISM survey. The clouds are classified into four different morphologies by visual inspection and using an automated algorithm – J plots. The visual inspection also serves as a test for the J plots algorithm, as this is the first time it has been used on molecular gas. Generally, it has been found that the structure of molecular clouds is highly filamentary and our observations indeed verify that most of our molecular clouds are elongated structures. Based on our visual classification of the 10663 SEDIGISM clouds, 15% are ring-like, 57% are elongated, 15% are concentrated and 10% are clumpy clouds. The remaining clouds do not belong to any of these morphology classes and are termed unclassified. We compare the SEDIGISM molecular clouds with structures identified through other surveys, i.e. ATLASGAL elongated structures and the bubbles from Milky Way Project (MWP). We find that many of the ATLASGAL and MWP structures are velocity coherent. ATLASGAL elongated structures overlap with ≈ 21% of the SEDIGISM elongated structures (elongated and clumpy clouds) and MWP bubbles overlap with ≈ 25% of the SEDIGISM ring-like clouds. We also analyse the starformation associated with different cloud morphologies using two different techniques. The first technique examines star formation efficiency (SFE) and the dense gas fraction (DGF), based on SEDIGISM clouds and ATLASGAL clumps data. The second technique uses the high-mass star formation (HMSF) threshold for molecular clouds. The results indicate that clouds with ring-like and clumpy morphologies show a higher degree of star formation.

Published
2022

17. The SEDIGISM survey: The influence of spiral arms on the molecular gas distribution of the inner Milky Way

Author

Colombo, D., Duarte-Cabral, A., Pettitt, A R, Urquhart, J.S., Wyrowski, F., Csengeri, T., Neralwar, K.R., Schuller, F., Menten, K.M., Anderson, L., Barnes, P., Beuther, H., Bronfman, L., Eden, D, Ginsburg, A, Henning, T., König, C., Lee, M.-Y., Mattern, M., Medina, S, Ragan, S.E., Rigby, A.J., Sanchez-Monge, A., Traficante, A., Yang, A. Y., Wienen, M., Colombo, D., Duarte-Cabral, A., Pettitt, A R, Urquhart, J.S., Wyrowski, F., Csengeri, T., Neralwar, K.R., Schuller, F., Menten, K.M., Anderson, L., Barnes, P., Beuther, H., Bronfman, L., Eden, D, Ginsburg, A, Henning, T., König, C., Lee, M.-Y., Mattern, M., Medina, S, Ragan, S.E., Rigby, A.J., Sanchez-Monge, A., Traficante, A., Yang, A. Y., and Wienen, M.

Abstract

The morphology of the Milky Way is still a matter of debate. In order to shed light on uncertainties surrounding the structure of the Galaxy, in this paper, we study the imprint of spiral arms on the distribution and properties of its molecular gas. To do so, we take full advantage of the SEDIGISM (Structure, Excitation, and Dynamics of the Inner Galactic Interstellar Medium) survey that observed a large area of the inner Galaxy in the 13CO (2-1) line at an angular resolution of 28". We analyse the influences of the spiral arms by considering the features of the molecular gas emission as a whole across the longitude–velocity map built from the full survey. Additionally, we examine the properties of the molecular clouds in the spiral arms compared to the properties of their counterparts in the inter-arm regions. Through flux and luminosity probability distribution functions, we find that the molecular gas emission associated with the spiral arms does not differ significantly from the emission between the arms. On average, spiral arms show masses per unit length of ⇠ 105 106 M kpc1. This is similar to values inferred from data sets in which emission distributions were segmented into molecular clouds. By examining the cloud distribution across the Galactic plane, we infer that the molecular mass in the spiral arms is a factor of 1.5 higher than that of the inter-arm medium, similar to what is found for other spiral galaxies in the local Universe. We observe that only the distributions of cloud mass surface densities and aspect ratio in the spiral arms show significant differences compared to those of the inter-arm medium; other observed differences appear instead to be driven by a distance bias. By comparing our results with simulations and observations of nearby galaxies, we conclude that the measured quantities would classify the Milky Way as a flocculent spiral galaxy, rather than as a grand-design one.

Published
2022

18. Contributors

Author

Anand, S.C., primary, Batcheller, J.C., additional, Chen, X., additional, Crown, E.M., additional, Govarthanam, K.K., additional, Hearle, J.W.S., additional, Holmes, D.A., additional, Horrocks, A.R., additional, Midha, V.K., additional, Mukhopadhyay, A., additional, Ogin, S.L., additional, Potluri, P., additional, Rajendran, S., additional, Rawal, A., additional, Rigby, A.J., additional, Shah, T.H., additional, Soin, N., additional, and Zhou, Y., additional

Published
2016
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20. Galactic Star Formation with NIKA2 (GASTON): Evidence of mass accretion onto dense clumps

Author

De Petris, M., Rigby, A.J., Adam, R., Ade, P., Ajeddig, H., Anderson, M., André, P., Artis, E., Aussel, H., Bacmann, A., Beelen, A., Benoît, A., Berta, S., Bing, L., Bourrion, O., Bracco, A., Calvo, M., Catalano, A., Désert, F.-X., Doyle, S., Driessen, E. F. C., García, P., Gomez, A., Goupy, J., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F., Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverría, M., Peretto, N., Perotto, L., Pisano, G., Ponthieu, N., Revéret, V., Ristorcelli, I., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., Watkins, E.J., Zylka, R., Ferragamo, A., Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Cardiff University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Massey University, Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Cryogénie (Cryo), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Cryogénie (NEEL - Cryo), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Physics, QC1-999, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, high redshift galaxy, Astrophysics - Astrophysics of Galaxies, star formation, millimetre observations, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

High-mass stars ($m_* \gtrsim 8 \, M_\odot$) play a crucial role in the evolution of galaxies, and so it is imperative that we understand how they are formed. We have used the New IRAM KIDs Array 2 (NIKA2) camera on the Institut de Radio Astronomie Millim\'{e}trique (IRAM) 30-m telescope to conduct high-sensitivity continuum mapping of $\sim2$ deg$^2$ of the Galactic plane (GP) as part of the Galactic Star Formation with NIKA2 (GASTON) large program. We have identified a total of 1467 clumps within our deep 1.15 mm continuum maps and, by using overlapping continuum, molecular line, and maser parallax data, we have determined their distances and physical properties. By placing them upon an approximate evolutionary sequence based upon 8 $\mu$m $\textit{Spitzer}$ imaging, we find evidence that the most massive dense clumps accrete material from their surrounding environment during their early evolution, before dispersing as star formation advances, supporting clump-fed models of high-mass star formation., Comment: To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences

Published
2022
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21. Exploring the millimetre emission in nearby galaxies: analysis of the edge-on galaxy NGC 891

Author

Katsioli, S., Adam, R., Ade, P., Ajeddig, H., André, P., Artis, E., Aussel, H., Beelen, A., Benoît, A., Berta, S., Bing, L., Bourrion, O., Calvo, M., Catalano, A., De Looze, I., De Petris, M., Désert, F.-X., Doyle, S., Driessen, E.F. C., Ejlali, G., Galametz, M., Galliano, F., Gomez, A., Goupy, J., Jones, A.P., Hughes, A., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F., Madden, S.C., Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverría, M., Nersesian, A., Perotto, L., Pisano, G., Ponthieu, N., Revéret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Smith, M. W. L., Tabatabaei, F., Tucker, C., Xilouris, E. M., Zylka, R., De Petris, M., Ferragamo, A., Mayet, F., Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, QC1-999, Astrophysics::High Energy Astrophysical Phenomena, General Engineering, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, millimetre observations, Physics and Astronomy, galaxies, cosmology, Astrophysics of Galaxies (astro-ph.GA), General Earth and Planetary Sciences, Astrophysics::Solar and Stellar Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, General Environmental Science
Abstract

New observations of the edge-on galaxy NGC 891, at 1.15 and 2 mm obtained with the IRAM 30-m telescope and the NIKA2 camera, within the framework of the IMEGIN (Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA2) Large Program, are presented in this work. By using multiwavelength maps (from the mid-IR to the cm wavelengths) we perform SED fitting in order to extract the physical properties of the galaxy on both global and local ($\sim$kpc) scales. For the interpretation of the observations we make use of a state-of-the-art SED fitting code, HerBIE (HiERarchical Bayesian Inference for dust Emission). The observations indicate a galaxy morphology, at mm wavelengths, similar to that of the cold dust emission traced by sub-mm observations and to that of the molecular gas. The contribution of the radio emission at the NIKA2 bands is very small (negligible at 1.15 mm and $\sim10\%$ at 2 mm) while it dominates the total energy budget at longer wavelengths (beyond 5 mm). On local scales, the distribution of the free-free emission resembles that of the dust thermal emission while the distribution of the synchrotron emission shows a deficiency along the major axis of the disc of the galaxy., To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences

Published
2021
Full Text
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22. Searching for high-z DSFGs with NIKA2 and NOEMA

Author

Bing, L., Adam, R., Ade, P., Ajeddig, H., André, P., Artis, E., Aussel, H., Beelen, A., Benoît, A., Berta, S., Béthermin, M., Bourrion, O., Calvo, M., Catalano, A., De Petris, M., Désert, F.-X., Doyle, S., Driessen, E.F.C., Gomez, A., Goupy, J., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F., Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverría, M., Neri, R., Omont, A., Perotto, L., Pisano, G., Ponthieu, N., Revéret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., Zylka, R., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)

Subjects
010308 nuclear & particles physics, Physics, QC1-999, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, high redshift galaxy, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, star formation, millimetre observations, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

As the possible progenitors of passive galaxies at z=2-3, dusty star-forming galaxies (DSFGs) at z>4 provide a unique perspective to study the formation, assembly, and early quenching of massive galaxies in the early Universe. The extreme obscuration in optical-IR makes (sub)mm spectral scans the most universal and unbiased way to confirm/exclude the high-z nature of candidate dusty star-forming galaxies. We present here the status of the NIKA2 Cosmological Legacy Survey (N2CLS), which is the deepest wide-area single-dish survey in the millimeter searching for high-z DSFGs. We also introduce a joint-analysis method to efficiently search for the spectroscopic redshift of high-z DSFGs with noisy spectra and photometric data and present its success in identifying the redshift of DSFGs found in NIKA2 science verification data., To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences

Published
2021
Full Text
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23. PSZ2 G091: A massive double cluster at $z\sim$ 0.822 observed by the NIKA2 camera

Author

Artis, E., Adam, R., Ade, P., Ajeddig, H., André, P., Arnaud, M., Aussel, H., Bartalucci, I., Beelen, A., Benoît, A., Berta, S., Bing, L., Bourrion, O., Calvo, M., Catalano, A., De Petris, M., Désert, F.-X., Doyle, S., Driessen, E.F.C., Ferragamo, A., Gomez, A., Goupy, J., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F., Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverrí, M., Paliwal, A., Perotto, L., Pisano, G., Pointecouteau, E., Ponthieu, N., Pratt, G.W., Revéret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., Yepes, G., Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; PSZ2 G091.83+26.11 is a massive galaxy cluster with M500 = 7.43 x 10^14 Msun at z = 0.822. This object exhibits a complex morphology with a clear bimodality observed in X-rays. However, it was detected and analysed in the Planck sample as a single, spherical cluster following a universal profile [1]. This model can lead to miscalculations of thermodynamical quantities, like the pressure profile. As future multiwavelength cluster experiments will detect more and more objects at higher redshifts (where we expect the fraction of merging objects to be higher), it is crucial to quantify this systematic effect. In this work, we use high-resolution observations of PSZ2 G091.83+26.11 by the NIKA2 camera to integrate the morphological characteristics of the cluster in our modelling. This is achieved by fitting a two-halo model to the SZ image and then by reconstruction of the resulting projected pressure profile. We then compare these results with the spherical assumption.

Published
2021

24. Overdensity of SubMillimiter Galaxies in the GJ526 Field mapped with the NIKA2 Camera

Author

Lestrade, J.-F., Adam, R., Ade, P., Ajeddig, H., Andre, P., Artis, E., Aussel, H., Beelen, A., Benoit, A., Berta, S., Bing, L., Bourrion, O., Calvo, M., Catalano, A., Coulais, A., de Petris, M., Desert, F.-X., Doyle, S., Driessen, E.F.C., Gomez, A., Goupy, J., Keruzore, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Macias-Perez, J.-.F., Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Munoz-Echeverria, M., Perotto, L., Pisano, G., Ponthieu, N., Reveret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., Zylka, R., Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)

Subjects
010308 nuclear & particles physics, Physics, QC1-999, FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, high redshift galaxy, 01 natural sciences, star formation, millimetre observations, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract

Using the NIKA2 dual band millimeter camera installed on the IRAM30m telescope, we have mapped a relatively large field (~70 arcmin^2) in the direction of the star GJ526 to investigate the nature of the sources found with the MAMBO camera at 1.2 mm ten years earlier. We have found that they must be dust-obscured galaxies (SMGs) in the background beyond the star. The new NIKA2 map at 1.15 mm reveals additional sources and, in fact, an overdensity of SMGs predominantly distributed along a filament-like structure in projection on the sky across the whole observed field. We speculate this might be a cosmic filament at high redshift as revealed in cosmological hydrodynamical simulations. Measurement of spectroscopic redshifts of the SMGs in the candidate filament is required now for a definitive confirmation of the nature of the structure., Comment: To appear in the Proceedings of the International Conference entitled mm Universe @ NIKA2, Rome (Italy), June 2021, EPJ Web of conferences

Published
2021
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25. Probing the role of magnetic fields in star-forming filaments: NIKA2-Pol commissioning results toward OMC-1

Author

De Petris, M., Ajeddig, H., Adam, R., Ade, P., André, P., Artis, E., Aussel, H., Beelen, A., Benoît, A., Berta, S., Bing, L., Bourrion, O., Calvo, M., Catalano, A., Désert, F.-X., Doyle, S., Driessen, E. F. C., Gomez, A., Goupy, J., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F., Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverría, M., Perotto, L., Pisano, G., Ponthieu, N., Revéret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., Zylka, R., Shimajiri, Y., Ferragamo, A., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Instituto de RadioAstronomía Milimétrica (IRAM), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, and École normale supérieure - Paris (ENS-PSL)

Subjects
010308 nuclear & particles physics, Physics, QC1-999, 0103 physical sciences, FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, 01 natural sciences
Abstract

Dust polarization observations are a powerful, practical tool to probe the geometry (and to some extent, the strength) of magnetic fields in star-forming regions. In particular, Planck polarization data have revealed the importance of magnetic fields on large scales in molecular clouds. However, due to insufficient resolution, Planck observations are unable to constrain the B-field geometry on prestellar and protostellar scales. The high angular resolution of 11.7 arcsec provided by NIKA2-Pol 1.15 mm polarimetric imaging, corresponding to $\sim$ 0.02 pc at the distance of the Orion molecular cloud (OMC), makes it possible to advance our understanding of the B-field morphology in star-forming filaments and dense cores (IRAM 30m large program B-FUN). The commissioning of the NIKA2-Pol instrument has led to several challenging issues, in particular, the instrumental polarization or intensity-to-polarization (leakage) effect. In the present paper, we illustrate how this effect can be corrected for, leading to reliable exploitable data in a structured, extended source such as OMC-1. We present a statistical comparison between NIKA2-Pol and SCUBA2-Pol2 results in the OMC-1 region. We also present tentative evidence of local pinching of the B-field lines near Orion-KL, in the form of a new small-scale hourglass pattern, in addition to the larger-scale hourglass already seen by other instruments such as Pol2., 6 pages, 3 figures, conference proceeding

Published
2022
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26. SEDIGISM-ATLASGAL: Dense Gas Fraction and Star Formation Efficiency Across the Galactic Disk

Author

Urquhart, J.S., Figura, C., Cross, J.R., Wells, M.R.A., Moore, T.J.T., Eden, D.J., Ragan, S.E., Pettitt, A.R., Duarte-Cabral, A., Colombo, D., Schuller, F., Csengeri, T., Mattern, M., Beuther, H., Menten, K.M., Wyrowski, F., Anderson, L.D., Barnes, P.J., Beltran, M.T., Billington, S.J., Bronfman, L., Giannetti, A., Kainulainen, J., Kauffmann, J., Lee, M.-Y., Leurini, S., Medina, S.-N. X., Montenegro-Montes, F.M., Riener, M., Rigby, A.J., Sanchez-Monge, A., Schilke, P., Schisano, E., Traficante, A., Wienen, M., Urquhart, J.S., Figura, C., Cross, J.R., Wells, M.R.A., Moore, T.J.T., Eden, D.J., Ragan, S.E., Pettitt, A.R., Duarte-Cabral, A., Colombo, D., Schuller, F., Csengeri, T., Mattern, M., Beuther, H., Menten, K.M., Wyrowski, F., Anderson, L.D., Barnes, P.J., Beltran, M.T., Billington, S.J., Bronfman, L., Giannetti, A., Kainulainen, J., Kauffmann, J., Lee, M.-Y., Leurini, S., Medina, S.-N. X., Montenegro-Montes, F.M., Riener, M., Rigby, A.J., Sanchez-Monge, A., Schilke, P., Schisano, E., Traficante, A., and Wienen, M.

Abstract

By combining two surveys covering a large fraction of the molecular material in the Galactic disk we investigate the role the spiral arms play in the star formation process. We have matched clumps identified by ATLASGAL with their parental GMCs as identified by SEDIGISM, and use these giant molecular cloud (GMC) masses, the bolometric luminosities, and integrated clump masses obtained in a concurrent paper to estimate the dense gas fractions (\(DGF_{gmc} = ∑M_{clump}/M_{gmc}\)) and the instantaneous star forming efficiencies (i.e., \(SFE_{gmc} = ∑L_{clump}/M_{gmc}\)). We find that the molecular material associated with ATLASGAL clumps is concentrated in the spiral arms (∼60 per cent found within ±10 km s\(^{−1}\) of an arm). We have searched for variations in the values of these physical parameters with respect to their proximity to the spiral arms, but find no evidence for any enhancement that might be attributable to the spiral arms. The combined results from a number of similar studies based on different surveys indicate that, while spiral-arm location plays a role in cloud formation and HI to H\(_2\) conversion, the subsequent star formation processes appear to depend more on local environment effects. This leads us to conclude that the enhanced star formation activity seen towards the spiral arms is the result of source crowding rather than the consequence of a any physical process.

Published
2020

28. List of contributors

Author

Anand, S.C., primary, Bajaj, P., additional, Byrne, C., additional, Chen, X., additional, Fung, W., additional, Gong, R.H., additional, Hall, M., additional, Hardman, E., additional, Holme, I., additional, Holmes, D., additional, Miraftab, M., additional, Ogin, S., additional, Pritchard, M., additional, Rankilor, P.R., additional, Rigby, A.J., additional, Sarsby, S.W., additional, Scott, R.A., additional, Slater, K., additional, Smith, P., additional, and Sondhelm, W., additional

Published
2000
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29. CHIMPS: Physical properties of molecular clumps across the inner Galaxy

Author

Rigby, A.J., Moore, T.J.T., Eden, D.J., Urquhart, J.S., Ragan, S.E., Peretto, N., Plume, R., Thompson, M.A., Currie, M.J., Park, G., Rigby, A.J., Moore, T.J.T., Eden, D.J., Urquhart, J.S., Ragan, S.E., Peretto, N., Plume, R., Thompson, M.A., Currie, M.J., and Park, G.

Abstract

The latest generation of high-angular-resolution unbiased Galactic plane surveys in molecular-gas tracers are enabling the interiors of molecular clouds to be studied across a range of environments. The CO Heterodyne Inner Milky Way Plane Survey (CHIMPS) simultaneously mapped a sector of the inner Galactic plane, within 27.8\(^\text{o}\) \(\lesssim\) \(\ell\) \(\lesssim\) 46.2\(^\text{o}\) and |\(\textit{b}\)| ≤ 0.5\(^{\rm o}\), in \({^1}{^3}\)CO (3–2) and C\({^1}{^8}\)O (3–2) at an angular resolution of 15 arcsec. The combination of the CHIMPS data with \({^1}{^2}\)CO (3–2) data from the CO High Resolution Survey (COHRS) has enabled us to perform a voxel-by-voxel local-thermodynamic-equilibrium (LTE) analysis, determining the excitation temperature, optical depth, and column density of \({^1}{^3}\)CO at each \(\ell\), \(\textit{b}\), \(\textit{v}\) position. Distances to discrete sources identified by FellWalker in the \({^1}{^3}\)CO (3–2) emission maps were determined, allowing the calculation of numerous physical properties of the sources, and we present the first source catalogues in this paper. We find that, in terms of size and density, the CHIMPS sources represent an intermediate population between large-scale molecular clouds identified by CO and dense clumps seen in thermal dust continuum emission, and therefore represent the bulk transition from the diffuse to the dense phase of molecular gas. We do not find any significant systematic variations in the masses, column densities, virial parameters, mean excitation temperature, or the turbulent pressure over the range of Galactocentric distance probed, but we do find a shallow increase in the mean volume density with increasing Galactocentric distance. We find that inter-arm clumps have significantly narrower linewidths, and lower virial parameters and excitation temperatures than clumps located in spiral arms. When considering the most reliable distance-limited subsamples, the largest variations occur on the

Published
2019

31. CHIMPS: The 13CO/C18O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey

Author

Rigby, A.J. Moore, T.J.T. Plume, R. Eden, D.J. Urquhart, J.S. Thompson, M.A. Mottram, J.C. Brunt, C.M. Butner, H.M. Dempsey, J.T. Gibson, S.J. Hatchell, J. Jenness, T. Kuno, N. Longmore, S.N. Morgan, L.K. Polychroni, D. Thomas, H. White, G.J. Zhu, M.

Abstract

We present the 13CO/C18O (J=3→2) Heterodyne Inner MilkyWay Plane Survey (CHIMPS) which has been carried out using the Heterodyne Array Receiver Program on the 15 m James Clerk Maxwell Telescope (JCMT) in Hawaii. The high-resolution spectral survey currently covers |b| ≤ 0°.5 and 28° ≲ l ≲ 46°, with an angular resolution of 15 arcsec in 0.5 km s-1 velocity channels. The spectra have amedian rms of~0.6 K at this resolution, and for optically thin gas at an excitation temperature of 10 K, this sensitivity corresponds to column densities of NH2 ~ 3 × 1020 cm-2 and NH2 ~ 4 × 1021 cm-2 for 13CO and C18O, respectively. The molecular gas that CHIMPS traces is at higher column densities and is also more optically thin than in other publicly available CO surveys due to its rarer isotopologues, and thus more representative of the three-dimensional structure of the clouds. The critical density of the J = 3 → 2 transition of CO is ≳104 cm-3 at temperatures of ≤20 K, and so the higher density gas associated with star formation is well traced. These data complement other existing Galactic plane surveys, especially the JCMT Galactic Plane Survey which has similar spatial resolution and column density sensitivity, and the Herschel infrared Galactic Plane Survey. In this paper, we discuss the observations, data reduction and characteristics of the survey, presenting integrated-emission maps for the region covered. Position-velocity diagrams allow comparison with Galactic structure models of the Milky Way, and while we find good agreement with a particular four-arm model, there are some significant deviations. © 2015 The Authors.

Published
2016

32. The JCMT Plane Survey: Early results from the ℓ = 30° field

Author

Moore, T.J.T. Plume, R. Thompson, M.A. Parsons, H. Urquhart, J.S. Eden, D.J. Dempsey, J.T. Morgan, L.K. Thomas, H.S. Buckle, J. Brunt, C.M. Butner, H. Carretero, D. Chrysostomou, A. deVilliers, H.M. Fich, M. Hoare, M.G. Manser, G. Mottram, J.C. Natario, C. Olguin, F. Peretto, N. Polychroni, D. Redman, R.O. Rigby, A.J. Salji, C. Summers, L.J. Berry, D. Currie, M.J. Jenness, T. Pestalozzi, M. Traficante, A. Bastien, P. diFrancesco, J. Davis, C.J. Evans, A. Friberg, P. Fuller, G.A. Gibb, A.G. Gibson, S. Hill, T. Johnstone, D. Joncas, G. Longmore, S.N. Lumsden, S.L. Martin, P.G. Nguyẽn Lu'o'ng, Q. Pineda, J.E. Purcell, C. Richer, J.S. Schieven, G.H. Shipman, R. Spaans, M. Taylor, A.R. Viti, S. Weferling, B. White, G.J. Zhu, M.

Abstract

We present early results from the JCMT (James Clerk Maxwell Telescope) Plane Survey (JPS), which has surveyed the northern inner Galactic plane between longitudes ℓ = 7° and ℓ = 63° in the 850-μm continuum with SCUBA-2 (Submm Common-User Bolometer Array 2), as part of the JCMT Legacy Survey programme. Data from the ℓ = 30° survey region, which contains the massive-star-forming regions W43 and G29.96, are analysed after approximately 40 per cent of the observations had been completed. The pixel-to-pixel noise is found to be 19 mJy beam-1 after a smooth over the beam area, and the projected equivalent noise levels in the final survey are expected to be around 10 mJy beam-1. An initial extraction of compact sourceswas performed using the FELLWALKER method, resulting in the detection of 1029 sources above a 5σ surface-brightness threshold. The completeness limits in these data are estimated to be around 0.2 Jy beam-1 (peak flux density) and 0.8 Jy (integrated flux density) and are therefore probably already dominated by source confusion in this relatively crowded section of the survey. The flux densities of extracted compact sources are consistent with those of matching detections in the shallower APEX (Atacama Pathfinder Experiment) Telescope Large Area Survey of the Galaxy (ATLASGAL) survey.We analyse the virial and evolutionary state of the detected clumps in the W43 star-forming complex and find that they appear younger than the Galactic-plane average. © 2015 The Authors.

Published
2015

33. Star formation scales and efficiency in Galactic spiral arms

Author

Eden, D.J., Moore, T.J.T., Urquhart, J.S., Elia, D., Plume, R., Rigby, A.J., Thompson, M.A., Eden, D.J., Moore, T.J.T., Urquhart, J.S., Elia, D., Plume, R., Rigby, A.J., and Thompson, M.A.

Abstract

We positionally match a sample of infrared-selected young stellar objects, identified by combining the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire, Wide-field Infrared Survey Explorer and Herschel Space Observatory Herschel infrared Galactic Plane Survey, to the dense clumps identified in the millimetre continuum by the Bolocam Galactic Plane Survey in two Galactic lines of sight centred towards l = 30° and 40°. We calculate the ratio of infrared luminosity, LIR, to the mass of the clump, Mclump, in a variety of Galactic environments and find it to be somewhat enhanced in spiral arms compared to the interarm regions when averaged over kiloparsec scales. We find no compelling evidence that these changes are due to the mechanical influence of the spiral arm on the star formation efficiency rather than, e.g. different gradients in the star formation rate due to patchy or intermittent star formation, or local variations that are not averaged out due to small source samples. The largest variation in LIR/Mclump is found in individual clump values, which follow a lognormal distribution and have a range of over three orders of magnitude. This spread is intrinsic as no dependence of LIR/Mclump with Mclump was found. No difference was found in the luminosity distribution of sources in the arm and interarm samples and a strong linear correlation was found between LIR and Mclump. © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2015

34. Optimisation of refractory lining design and installation practice to reduce vessel downtime and maximise performance of anode refining vessels.

Author

Rigby A.J., Cu2007; John E. Dutrizac symposium on copper hydrometallurgy, Toronto, Ontario, 25-30 Aug. 2007, Richeson C., Wiessler M.P., Rigby A.J., Cu2007; John E. Dutrizac symposium on copper hydrometallurgy, Toronto, Ontario, 25-30 Aug. 2007, Richeson C., and Wiessler M.P.

Abstract

Modern anode vessel relining methods, using roller-conveyor delivery through access doors in the endwall and T plates to anchor and support the lining bricks during installation, can reduce re-lining time by more than 50% and double lining life., Modern anode vessel relining methods, using roller-conveyor delivery through access doors in the endwall and T plates to anchor and support the lining bricks during installation, can reduce re-lining time by more than 50% and double lining life.

Published
2007

35. Effect of Ginkgo biloba (EGb 761) and aspirin on platelet aggregation and platelet function analysis among older adults at risk of cardiovascular disease: a randomized clinical trial

Author

Gardner, C.D., Zehnder, J.L., and Rigby, A.J.

Subjects
Aspirin -- Dosage and administration -- Usage -- Research, Cardiovascular diseases -- Research -- Risk factors -- Drug therapy, Ginkgo -- Usage -- Health aspects -- Research, Health, Drug therapy, Usage, Research, Risk factors, Dosage and administration, Health aspects
Abstract

Several case reports have implicated Ginkgo biloba in clinically adverse bleeding disorders. Ginkgo biloba has been reported to increase pain-free walking distance among patients with peripheral artery disease (PAD). Standard [...]

Published
2008

40. Refractory performance in Peirce-Smith converters at BHP San Manuel smelter.

Author

Gonzales T.W., Copper 99 - Cobre 99 international conference Phoenix, Arizona 10-Oct-9913-Oct-99, Pasca O., Rigby A.J., Gonzales T.W., Copper 99 - Cobre 99 international conference Phoenix, Arizona 10-Oct-9913-Oct-99, Pasca O., and Rigby A.J.

Abstract

Over the last four years, considerable improvements in tuyere lining life have been achieved at the Arizona copper smelter by maintaining a uniform temperature in the operating converter and ensuring that there is sufficient and specific allowance for expansion in the construction of the refractory brickwork. A combination of optimised crane availability, rapid matte transfer, improved converter operating practices, new refractory applications and new installation techniques has minimised down-time. In addition, the use of large-diameter tuyere pipes and hard piping have increased blowing rates and reduced cycle times, resulting in more than 62 500 tonnes of blister copper being produced before new tuyere linings were required. The new brick installation technique is described and illustrated., Over the last four years, considerable improvements in tuyere lining life have been achieved at the Arizona copper smelter by maintaining a uniform temperature in the operating converter and ensuring that there is sufficient and specific allowance for expansion in the construction of the refractory brickwork. A combination of optimised crane availability, rapid matte transfer, improved converter operating practices, new refractory applications and new installation techniques has minimised down-time. In addition, the use of large-diameter tuyere pipes and hard piping have increased blowing rates and reduced cycle times, resulting in more than 62 500 tonnes of blister copper being produced before new tuyere linings were required. The new brick installation technique is described and illustrated.

Published
1999

41. Use of microporous insulation in copper holding furnaces at BHP Copper, San Manuel, AZ.

Author

Mackenzie I.B., Copper 99 - Cobre 99 international conference Phoenix, Arizona 10-Oct-9913-Oct-99, Enriquez A., Pasca O., Rigby A.J., Mackenzie I.B., Copper 99 - Cobre 99 international conference Phoenix, Arizona 10-Oct-9913-Oct-99, Enriquez A., Pasca O., and Rigby A.J.

Abstract

In 1997, a thin layer of Microtherm microporous insulation was used to replace fireclay bricks behind the magnesia/chrome working lining in No.5 refining furnace at the Arizona smelter. A reduction in shell temperature of 23 degrees C was obtained, together with a large increase in the working capacity of the vessel. There was no sign of metal penetration as a result of the increased insulation. Following these highly favourable results, BHP introduced the product into all their refining furnaces., In 1997, a thin layer of Microtherm microporous insulation was used to replace fireclay bricks behind the magnesia/chrome working lining in No.5 refining furnace at the Arizona smelter. A reduction in shell temperature of 23 degrees C was obtained, together with a large increase in the working capacity of the vessel. There was no sign of metal penetration as a result of the increased insulation. Following these highly favourable results, BHP introduced the product into all their refining furnaces.

Published
1999

42. Porous plugs in molten copper production and refining.

Author

Rigby A.J., Copper 99 - Cobre 99 international conference Phoenix, Arizona 10-Oct-9913-Oct-99, Lanyi M.D., Rigby A.J., Copper 99 - Cobre 99 international conference Phoenix, Arizona 10-Oct-9913-Oct-99, and Lanyi M.D.

Abstract

The current use of porous plugs to inject nitrogen into molten copper during primary smelting is described. Nitrogen stirring increases heat transfer to the bath, eliminates temperature stratification and improves efficiency during desulphurisation and deoxidation. The possibility of using porous plugs to introduce reducing gases for deoxidising copper is also discussed: previously reported laboratory results point to very high efficiency of hydrogen utilisation for such reduction. Of the various designs available, the permeable 95% magnesia plug has proved most effective and least prone to blockage by frozen metal during loss of nitrogen pressure. To minimise erosion, the plug is seated in a nest-block, which may allow external removal of the plug for replacement. The possibility of using plugs for successive injection of air, nitrogen and hydrogen is considered., The current use of porous plugs to inject nitrogen into molten copper during primary smelting is described. Nitrogen stirring increases heat transfer to the bath, eliminates temperature stratification and improves efficiency during desulphurisation and deoxidation. The possibility of using porous plugs to introduce reducing gases for deoxidising copper is also discussed: previously reported laboratory results point to very high efficiency of hydrogen utilisation for such reduction. Of the various designs available, the permeable 95% magnesia plug has proved most effective and least prone to blockage by frozen metal during loss of nitrogen pressure. To minimise erosion, the plug is seated in a nest-block, which may allow external removal of the plug for replacement. The possibility of using plugs for successive injection of air, nitrogen and hydrogen is considered.

Published
1999

44. The COP KIN system: performance and benefits, a world-wide overview.

Author

Filzwieser A., Caulfield K., Rigby A.J., Wallner S., Filzwieser A., Caulfield K., Rigby A.J., and Wallner S.

Abstract

The use of gas stirring systems with porous plugs is now widespread in the aluminium and copper industries. The paper describes the use of plugs, and the new standardised gas stirring COP KIN system for nitrogen stirring of molten copper. The metallurgical benefits of the system in anode furnace operation include a uniform bath temperature, less slag overheating, prevention of build-up, efficient removal of slag and undesirable elements, process time reduction, and lower and more uniform final oxygen content in the cast anode. Some brief examples of gas stirring systems are given., The use of gas stirring systems with porous plugs is now widespread in the aluminium and copper industries. The paper describes the use of plugs, and the new standardised gas stirring COP KIN system for nitrogen stirring of molten copper. The metallurgical benefits of the system in anode furnace operation include a uniform bath temperature, less slag overheating, prevention of build-up, efficient removal of slag and undesirable elements, process time reduction, and lower and more uniform final oxygen content in the cast anode. Some brief examples of gas stirring systems are given.

45. Wear mechanisms for refractory linings.

Author

Rigby A.J. and Rigby A.J.

Abstract

Peirce Smith converters, Hoboken converters and anode furnaces are universally lined with magnesite and chromite refractories. Rapid wear in the tuyere zone results from contact with agitated silicate slags rich in iron oxide and from permanent changes in tuyere temperature and cleanliness. Typical chemical and physical properties of magnesite-chrome refractories used in converter and anode furnace tuyeres and in the converter itself are compared. Operational factors contributing to their wear include the environment in the tuyere zone, the effect of matte grade, which can vary from 40% to 75%, the length of time between blows, control of slag temperature and chemical composition, and tuyere punching/cleaning practice. Other factors are related to refractory installation practice and the quality and microstructural properties of the refractory bricks., Peirce Smith converters, Hoboken converters and anode furnaces are universally lined with magnesite and chromite refractories. Rapid wear in the tuyere zone results from contact with agitated silicate slags rich in iron oxide and from permanent changes in tuyere temperature and cleanliness. Typical chemical and physical properties of magnesite-chrome refractories used in converter and anode furnace tuyeres and in the converter itself are compared. Operational factors contributing to their wear include the environment in the tuyere zone, the effect of matte grade, which can vary from 40% to 75%, the length of time between blows, control of slag temperature and chemical composition, and tuyere punching/cleaning practice. Other factors are related to refractory installation practice and the quality and microstructural properties of the refractory bricks.

46. Searching for high-z DSFGs with NIKA2 and NOEMA

Author

Bing, L., Adam, R., Ade, P., Ajeddig, H., André, P., Artis, E., Aussel, H., Beelen, A., Benoit, A., Berta, S., Béthermin, M., Bourrion, O., Calvo, M., Catalano, A., De Petris, M., Désert, F.-X., Doyle, S., Driessen, E.F.C., Gomez, A., Goupy, J., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F, Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverría, M., Neri, R., Omont, A., Perotto, L., Pisano, G., Ponthieu, N., Revéret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., Zylka, R., Bing, L., Adam, R., Ade, P., Ajeddig, H., André, P., Artis, E., Aussel, H., Beelen, A., Benoit, A., Berta, S., Béthermin, M., Bourrion, O., Calvo, M., Catalano, A., De Petris, M., Désert, F.-X., Doyle, S., Driessen, E.F.C., Gomez, A., Goupy, J., Kéruzoré, F., Kramer, C., Ladjelate, B., Lagache, G., Leclercq, S., Lestrade, J.-F., Macías-Pérez, J.-F, Maury, A., Mauskopf, P., Mayet, F., Monfardini, A., Muñoz-Echeverría, M., Neri, R., Omont, A., Perotto, L., Pisano, G., Ponthieu, N., Revéret, V., Rigby, A.J., Ritacco, A., Romero, C., Roussel, H., Ruppin, F., Schuster, K., Shu, S., Sievers, A., Tucker, C., and Zylka, R.

Abstract

As the possible progenitors of passive galaxies at z=2-3, dusty starforming galaxies (DSFGs) at z>4 provide a unique perspective to study the formation, assembly, and early quenching of massive galaxies in the early Universe. The extreme obscuration in optical-IR makes (sub)mm spectral scans the most universal and unbiased way to confirm/exclude the high-z nature of candidate dusty star-forming galaxies. We present here the status of the NIKA2 Cosmological Legacy Survey (N2CLS), which is the deepest wide-area singledish survey in the millimeter searching for high-z DSFGs. We also introduce a joint-analysis method to effciently search for the spectroscopic redshift of high-z DSFGs with noisy spectra and photometric data and present its success in identifying the redshift of DSFGs found in NIKA2 science verification data....

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