Si ricorda che gli Associati INAF (Esterni, quali ad esempio personale universitario) NON devono confermare le proprie FTE. Gli associati hanno facoltà di leggere la scheda INAF nella parte pubblica senza necessità di account.
Scheda FQS
FINAL
Scheda convalidata, con Checksum 4c1e5facde38fcc3e4b234372bd3337632ac3e7197074ea22a7bbee106bf01a6
FQS è un programma basato su 700 ore di osservazione di 12CO(1-0) and 13CO(1-0) in 50 gradi quadrati del piano della Via Lattea (220°<l<240°, -2.5°<b<0°) con l'antenna di 12m del Arizona Radio Observatory. Questi dati hanno rivelato la disposizione del gas molecolare in strutture sempre più dense e piccole, partendo dai bracci a spirale, definiti dalle nubi molecolari giganti, con la loro rete di filamenti, fino ai clumps e cores dove si formano le stelle. Il dataset di FQS, con il suo grande valore di legacy, ha notevolmente aumentato la qualità dei dati molecolari disponibili in precedenza. Nei dati di FQS si possono identificare strutture molecolari a varie scale spaziali e derivarne la distanza , ottenendo cosi stime corrette di parametri fisici essenziali quali dimensione e massa.
FQS is a large program that used 700 hr of the 12m antenna at the Arizona Radio Observatory to map 50 square degree of the Milky Way plane (220°<l<240°, -2.5°<b<0°) in 12CO(1-0) and 13CO(1-0). These data have shown how the molecular dense gas is organised at different spatial scales: from spiral arms traced by the giant clouds with their denser filamentary networks, down to the clumps and cores that host the new-born stars. FQS produced a dataset of great legacy value, largely improving the quality of both sensitivity and spatial resolution over previous data sets. From these high-quality spectroscopic data we can identify molecular structures at different scales and derive the distance of the emitting gas, obtaining reliable estimates of key physical parameters such as size and mass.
Mezzo interstellare, formazione di stelle e sistemi planetari
Infrastrutture da Terra (utilizzo)
Infrastrutture dallo spazio per l’osservazione dell Universo (utilizzo)
15. Team Summary
15. Personale INAF coinvolto
Numero di partecipanti INAF al progetto: 12
Struttura
Nfte
N0
TI 2024
TI 2025
TI 2026
TD 2024
TD 2025
TD 2026
Nex
Extra
IAPS ROMA
1
0
0.20
0.20
0.00
0
0
0
1
0.10
O.A. ARCETRI
0
0
0.00
0.00
0.00
0
0
0
0
0.00
IRA BOLOGNA
0
0
0.00
0.00
0.00
0
0
0
0
0.00
Totali
1
0
0.20
0.20
0.00
0.00
0.00
0.00
1
0.10
16. Personale Associato INAF coinvolto
Numero di partecipanti Associati INAF: 1
#
Struttura
TI 2024
TI 2025
TI 2026
TD 2024
TD 2025
TD 2026
Extra
1
UniBo - O.A. Arcetri
0.00
0.00
0.00
0
0
0
0.00
Totali
0.00
0.00
0.00
0.00
0.00
0.00
0.00
Fondi a sostegno
21. Totale fondi a disposizione (dato aggregato, k€)
Certi 2024
Certi 2025
Certi 2026
Presunti 2024
Presunti 2025
Presunti 2026
0
0
0
0
0
0
Produzione scientifica e tecnologica
22. Produzione scientifica e tecnologica - Highlights
#
DOI
Descrizione
Azione
1
10.1051/0004-6361/201936096
titolo: The Forgotten Quadrant Survey. 12CO and 13CO (1-0) survey of the Galactic plane in the range 220° <l <240° -2.°5 < b < 0°
autori: Benedettini, M.; Molinari, S.; Baldeschi, A.; Beltrán, M. T.; Brand, J.; Cesaroni, R.; Elia, D.; Fontani, F.; Merello, M.; Olmi, L.; Pezzuto, S.; Rygl, K. L. J.; Schisano, E.; Testi, L.; Traficante, A.
Abstract:
Aims: We present the Forgotten Quadrant Survey (FQS), an ESO large project that used the 12 m antenna of the Arizona Radio Observatory to map the Galactic plane in the range 220° < l < 240° and -2.°5 < b < 0°, both in 12CO (1-0) and 13CO (1-0), at a spectral resolution of 0.65 km s-1 and 0.26 km s-1.
Methods: We used the (1-0) transition of carbon monoxide to trace the molecular component of the interstellar medium. Our data set allows us to easily identify how the molecular dense gas is organised at different spatial scales: from the giant clouds with their denser filamentary networks, down to the clumps and cores that host the new-born stars and to obtain reliable estimates of their key physical parameters such as size and mass.
Results: We present the first release of the data of the FQS survey and discuss their quality. Spectra with 0.65 km s-1 velocity channels have noise ranging from 0.8 K to 1.3 K for 12CO (1-0) and from 0.3 K to 0.6 K for 13CO (1-0). In this first paper, we used the 12CO (1-0) spectral cubes to produce a catalogue of 263 molecular clouds. The clouds are grouped in three main structures corresponding to the Local, Perseus, and Outer arms up to a distance of ˜8.6 kpc from the Sun. This is the first self-consistent statistical catalogue of molecular clouds of the outer Galaxy obtained with a subarcminute spatial resolution and therefore able to detect not only the classical giant molecular clouds, but also the small clouds and to resolve the cloud structure at the sub-parsec scale up to a distance of a few kiloparsec. We found two classes of objects: structures with sizes above a few parsecs that are typical molecular clouds and may be self-gravitating, and subparsec structures that cannot be in gravitational equilibrium and are likely transient or confined by external pressure. We used the ratio between the Herschel H2 column density and the integrated intensity of the CO lines to calculate the CO conversion factor and we found mean values of (3.3 ± 1.4) × 1020 cm-2 (K km s-1)-1 and (1.2 ± 0.4) × 1021 cm-2 (K km s-1)-1, for 12CO (1-0) and 13CO (1-0), respectively.
Conclusions: The FQS contributes to the general effort in producing a new generation of high-quality spectroscopic data for the Galactic plane in the less-studied third Galactic quadrant toward the outer Galaxy. The FQS has produced a data set of great legacy value, largely improving the data quality both in terms of sensitivity and spatial resolution over previous data sets.
2
10.1051/0004-6361/202141433
Molecular cloud catalogue from 13CO (1-0) data of the Forgotten Quadrant Survey
Benedettini, M.; Traficante, A.; Olmi, L.; Pezzuto, S.; Baldeschi, A. ; Molinari, S. ; Elia, D.; Schisano, E.; Merello, M.; Fontani, F; Rygl, K. L. J.; Brand, J.; Beltrán, M. T.; Cesaroni, R.; Liu, S. J. ; Testi, L.
Abstract
Context. New-generation spectroscopic surveys of the Milky Way plane have been revealing the structure of the interstellar medium, allowing the simultaneous study of dense structures from single star-forming objects or systems to entire spiral arms.
Aims: The good sensitivity of the new surveys and the development of dedicated algorithms now enable building extensive catalogues of molecular clouds and deriving good estimates of their physical properties. This allows studying the behaviour of these properties across the Galaxy.
Methods: We present the catalogue of molecular clouds extracted from the 13CO (1-0) data cubes of the Forgotten Quadrant Survey, which mapped the Galactic plane in the range 220° < l < 240° and −2.° 5 < b < 0° in 12CO (1-0) and 13CO (1-0). We compared the properties of the clouds of our catalogue with those of other catalogues.
Results: The catalogue contains 87 molecular clouds for which the main physical parameters such as area, mass, distance, velocity dispersion, and virial parameter were derived. These structures are overall less extended and less massive than the molecular clouds identified in the 12CO (1-0) data-set because they trace the brightest and densest part of the 12CO (1-0) clouds. Conversely, the distribution of aspect ratio, equivalent spherical radius, velocity dispersion, and virial parameter in the two catalogues are similar. The mean value of the mass surface density of molecular clouds is 87 ± 55 M⊙ pc−2 and is almost constant across the galactocentric radius, indicating that this parameter, which is a proxy of star formation, is mostly affected by local conditions.
Conclusions: In data of the Forgotten Quadrant Survey, we find a good agreement between the total mass and velocity dispersion of the clouds derived from 12CO (1-0) and 13CO (1-0). This is likely because in the surveyed portion of the Galactic plane, the H2 column density is not particularly high, leading to a CO emission with a not very high optical depth. This mitigates the effects of the different line opacities between the two tracers on the derived physical parameters. This is a common feature in the outer Galaxy, but our result cannot be readily generalised to the entire Milky Way because regions with higher particle density could show a different behaviour.
3
10.48550/arXiv.2403.00512
titolo: Cloud properties across spatial scales in simulations of the interstellar medium. Autori: Colman, Tine ; Brucy, Noé search by orcid ; Girichidis, Philipp ; Glover, Simon C. O ; Benedettini, Milena ; Soler, Juan D. ; Tress, Robin G. ; Traficante, Alessio ; Hennebelle, Patrick ; Klessen, Ralf S. ; Molinari, Sergio ; Miville-Deschênes, Marc-Antoine. Abstract: Molecular clouds (MC) are structures of dense gas in the interstellar medium (ISM), that extend from ten to a few hundred parsecs and form the main gas reservoir available for star formation. Hydrodynamical simulations of varying complexity are a promising way to investigate MC evolution and their properties. However, each simulation typically has a limited range in resolution and different cloud extraction algorithms are used, which complicates the comparison between simulations. In this work, we aim to extract clouds from different simulations covering a wide range of spatial scales. We compare their properties, such as size, shape, mass, internal velocity dispersion and virial state. We apply the Hop cloud detection algorithm on (M)HD numerical simulations of stratified ISM boxes and isolated galactic disk simulations that were produced using Flash Ramses and Arepo We find that the extracted clouds are complex in shape ranging from round objects to complex filamentary networks in all setups. Despite the wide range of scales, resolution, and sub-grid physics, we observe surprisingly robust trends in the investigated metrics. The mass spectrum matches in the overlap between simulations without rescaling and with a high-mass slope of dN/dlnM∝−1 in accordance with theoretical predictions. The internal velocity dispersion scales with the size of the cloud as σ∝R^0.75 for large clouds (R≳3pc). For small clouds we find larger sigma compared to the power-law scaling, as seen in observations, which is due to supernova-driven turbulence. Almost all clouds are gravitationally unbound with the virial parameter scaling as αvir∝M^−0.4, which is slightly flatter compared to observed scaling, but in agreement given the large scatter.