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Franco, Raquel Campos; Wang, Lili; O’Rourke, Pauric; Breeze, Beth; Künzl, Jan; Govekar, Chris; Biggers, Christopher S.; Bour, Odile; Hölz, Martin; List, Regina; Real, Carlos Cordourier; Kraeger, Patsy; Lingelbach, Gabriele; O’Halloran, Kerry; Pospı́šil, Miroslav; Griffin, Christopher L.; Robichau, Robbie Waters; Liedhegener, Antonius; Martı́nez, Francisco; Gosewinkel, Dieter; Moro, Giovanni; Fowler, Alan; Halman, Loek; Dacombe, Rod; Levi, Elizabeth; Irish, Leon E.; Lange, Dirk; Isar, Yudhishthir Raj; Howard, Marc Morjé; Romanienko, Lisiunia A.; Reynolds, Travis; Seckinelgin, Hakan; Juergensmeyer, Mark; Lyons, Mark; Nowland-Foreman, Garth; Filho, Marco Antonio Figueiredo Milani; Viana, Marcia Serra Ribeiro; Czike, Klára; Yachkaschi, Schirin; Toogood-Luehrs, Kimairis; Chan, Kin-man; Kanyinga, Karuti; Tsujinaka, Yutaka; Park, Tae-Kyu; Hwang, Chang-Soon; Natal, Alejandro; Cadena-Roa, Jorge; Rappoport, Sara Gordon; Liverani, Andrea; Gilbert, Leah; Sivesind, Karl Henrik; Selle, Per; Roitter, Mario; Blomkvist, Hans; Uba, Katrin; Weiss, Meredith; Boje, Thomas P.; Saber, Alaa; Milofsky, Carl; Klie, Thomas; Kocka, Jürgen; Brauer, Kai; Kohler‐Koch, Beate; Rajagopal, Arvind; Molnár, Gábor; Sarles, Curtis; Davies, Thomas; Bauerkämper, Arnd; Kostovicova, Denisa; Heinrich, V. Finn; Sulek, Marty; Mukherjee, Dhrubodhi; Kuruvilla, Shyama; Malešević, Siniša; Malešević, Vesna; Katz, Hagai; Rucht, Dieter; Schmidt, Jürgen; Puga, Cristina; Klein, Ansgar; Powell, Fred; Opitz-Belakhal, Claudia; Adloff, Frank; Hill, Lisa; Brinton, Aspen; Obadare, Ebenezer; Keane, John; Meyer, Megan; Stacey, Simon; Austin, James E.; Ebrahim, Alnoor; Anheier, Helmut K.; Krieger, Kristian; Gugerty, Mary Kay; Lotz, Jim; Fox, Jonathan; Vrielink, Mirjan Oude; Montfort, Cor van; Marx, Johannes; Pfaff, Steve; Valdez, Sarah; Labigne, Anael; Tuckman, Howard P.; Schortgen, Alicia; Turnour, Matthew; McGregor-Lowndes, Myles; Lohmann, Roger A.; Etzioni, Amitaï; Park, Sang Peel; McQuarrie, Michael; Cumming, Lawrence S.; Hale, Sharilyn; Spear, Roger; Zhu, Xiaoyan; Knoke, David; Douglas, Heather; Yunis, Feisal A.; Eck, Steve Van; Rehli, Florian; Smith, Steven Rathgeb; Jones, Derek C.; Kalmi, Panu; Altman, Morris; Nährlich, Stefan; Filipovitch, Anthony; Moore, Jessica; Stephenson, Max; Croce, Mariano; Reaves, Allyson; MacPherson, Ian; Brainard, Lori A.

doi:10.1007/978-0-387-93996-4_543

Cited by 1 publication

(1 citation statement)

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“…The distance uncertainties are adopted from following papers: Aquila (Straižys et al 2003); AurigaN and Auriga (Lada et al 2009); Cepheus 1, 3, and 5 (Kirk et al 2009); Cham I and III (Belloche et al 2011); Cham II (Whittet et al 1997); CoronaAus. (Neuhäuser & Forbrich 2008); IC5146E and NW (Harvey et al 2008); Lupus I, III-VI (Comerón 2008); Musca (Knude & Hog 1998;Franco 1991;Cox et al 2016); Ophiuchus (de Geus et al 1989); OphNorth1, 3, and 6 (Wilking et al 2008;Hatchell et al 2012); Perseus (Enoch et al 2006); Serpens (Dzib et al 2010(Dzib et al , 2011. Ragan et al (2014), Wang et al (2015), and Abreu-Vicente et al…”

Section: Discussionmentioning

confidence: 99%

Star-forming content of the giant molecular filaments in the Milky Way

Zhang

Kainulainen

Mattern

et al. 2019

A&A

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Context. Observations have discovered numerous giant molecular filaments (GMFs) in the Milky Way. Their role in the Galactic star formation and Galaxy-scale evolution of dense gas is unknown. Aims. We investigate systematically the star-forming content of all currently known GMFs. This allows us to estimate the star formation rates (SFRs) of the GMFs and to establish relationships between the SFRs and the GMF properties. Methods. We identify and classify the young stellar object (YSO) population of each GMF using multi-wavelength photometry from near-to far-infrared. We estimate the total SFRs assuming a universal and fully sampled initial mass function and luminosity function. Results. We uniformly estimate the physical properties of 57 GMFs. The GMFs show correlations between the 13 CO line width, mass, and size, similar to Larson's relations. We identify 36 394 infrared excess sources in 57 GMFs and obtain SFRs for 46 GMFs. The median SFR surface density (Σ SFR ) and star formation efficiency (SFE) of GMFs are 0.62 M Myr −1 pc −2 and 1%, similar to the nearby star-forming clouds. The star formation rate per free-fall time of GMFs is between 0.002−0.05 with the median value of 0.02. We also find a strong correlation between SFR and dense gas mass that is defined as gas mass above a visual extinction of 7 mag, which suggests that the SFRs of the GMFs scale similarly with dense gas as those of nearby molecular clouds. We also find a strong correlation between the mean SFR per unit length and dense gas mass per unit length. The origin of this scaling remains unknown, calling for further studies that can link the structure of GMFs to their SF activity and explore the differences between GMFs and other molecular clouds.

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