The ATLASGAL catalogue of class I methanol masers Silvia Leurini - PowerPoint PPT Presentation

The ATLASGAL catalogue of class I methanol masers Silvia Leurini INAF OA-Cagliari The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Outlook • CH 3 OH masers • Observational properties of Class I CH 3 OH masers • Bright Class I CH 3 OH masers:… what are they good for? • The ATLASGAL catalogue of Class I methanol masers 2 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Methanol masers Class II methanol (CH 3 OH) masers Class I methanol (CH 3 OH) masers • Located in the nearest vicinity of YSOs • Scattered around YSOs (up to a parsec) • IR radiation excitation from a massive • Collisional excitation YSO • astrophysical shocks • Regions of high mass star formation only G023.01-00.41 Navarete+in prep. Navarete+in prep. ✕ ✕ CO(6-5)+ Spitzer CO(6-5)+ Spitzer Voronkov+2006 Sanna+2015 3 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Class I masers: Pumping mechanisms Class I methanol (CH 3 OH) masers • First detection in the J k=2 − J k=1 E at 25 GHz in the late ‘80s, followed by the brighter 7 0 − 6 1 -A+ and 4 -1 − 3 0 -E lines at 44 and 36 GHz (Barrett+1971, Morimoto+1985) • (J+1) -1 − J 0 -E/(J+1) 0 − J 1 -A type series: t heir occurrence can be explained from the basic properties of the molecule (i.e. collisional rates and selection rules) ✕ • J 2 − J 1 -E series: ad hoc additional preference for the Δ k = ✕ ✕ 3 collisions over Δ k = 2 (Johnston+1992), or totally ✕ unselective collisions (Cragg+1992) collisional rates with large set of levels and H 2 as collisional partner computed by Rabli & Flower 2010ab, 2011 ⇒ Working model for bright Class I masers (Leurini, Menten, Walmsley 2016) (a) (b) 4 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Class I masers… what are they good for? Class I masers have typical luminosities of ~ 10 -6 L ⊙ ⇒ completely unimportant energetically compared to Class II masers (L>10 -6 L ⊙ and up to 10 -3 L ⊙ , Pestalozzi+2007) • signposts of interaction regions of shocks with dense ambient material • efficient outflow tracers, unaffected by extinction and strong at mm wavelengths ⇒ potentially a powerful tool for protostellar activity in extremely embedded objects • extremely sensitive to the physics of the emitting gas ⇒ multiline studies can constrain the temperature and density structure of outflows NOEMA 84 GHz ✕ ✕ and…we have a working model for bright Class I masers! ✕ Pihlström +2014 Voronkov+2010 Sobolev+1992,Salii+2002 Gómez-Ruiz+in prep. outflows cloud-cloud collision SNRs expanding HII region HM: Plambeck & Menten 1990+ Sobolev+1992+ Yusef-Zadeh+2008+ Voronkov+2010,2014 LM: Kalenskii et al. 2010a,b 5 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

The ATLASGAL catalogue of Class I methanol masers 70 µm weak 24 µm dark 24 µm bright 24 µm bright+cm time evolution Csengeri, Leurini+2016 Spitzer 3.6µm (blue), 8µm(green), and WISE 22µm (red) 200 massive clumps in four evolutionary phases of massive SF: • 70 µm-weak clumps with no embedded point-like source ⇒ candidates starless/prestellar sources • 24 µm-quiet clumps with compact point sources at 70 µm ⇒ sources in early protostellar phase • MIR-bright clumps with embedded YSOs strong at 8 µm and 24 µm ⇒ sources hosting YSOs • MIR-bright clumps with cm continuum emission ⇒ sources associated with a UCHII region 6 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Effelsberg: • 4 -1 → 3 0 -E @ 36.2 GHz • 7 0 → 6 1 -A @ 44.1 GHz • Full sample observed • Δ v=0.1 kms -1 credits MPIfR SRT: • J 2 − J 1 series @ 25 GHz • low Δ v (1.2 kms -1 ) survey of ~ 60 sources • high Δ v (0.02 kms -1 ) deep integration on detections credits IRAM credits INAF IRAM 30m: • 3mm line survey including 5 -1 → 4 0 -E @ 84.5 GHz 8 0 → 7 1 -A @ 95.1 GHz • Full sample • Δ v=0.7 kms -1 7 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

The ATLASGAL catalogue of class I methanol masers 70 µm weak 24 µm dark 24 µm bright 24 µm bright+cm 95 GHz S(Jy) 84 GHz S(Jy) 44 GHz S(Jy) 36 GHz S(Jy) 25 GHz X(counts) 8 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

The ATLASGAL catalogue of class I methanol masers *essentially as the 44GHz line but data Detection rates under examination *poor statistics 25 GHz 36 GHz * 44 GHz 84 GHz 95 GHz 37% 70% 33% 57% Total — 44% 44% 17% 22% 70 µm weak 14%* 73% 73% 34% 60% 24 µm dark 30% 71% 71% 39% 64% 24 µm bright 24 µm bright 52% 75% 75% 31% 58% +cm 9 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

The ATLASGAL catalogue of class I methanol masers *essentially as the 44GHz line but data Detection rates under examination *poor statistics 25 GHz 36 GHz * 44 GHz 84 GHz 95 GHz 37% 70% 33% 57% Total — 44% 44% 17% 22% 70 µm weak ⇒ at least 44% of the prestellar candidates already host molecular outflows 14%* 73% 73% 34% 60% 24 µm dark 30% 71% 71% 39% 64% 24 µm bright 24 µm bright 52% 75% 75% 31% 58% +cm 10 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Class I masers in ATLASGAL selected sources G014.4918 − 0.1389 WISE + 870 m Contours G14.49-0.14 95 GHz maser 2 1 84 GHz maser 0 44 GHz maser − 1 − 2 36 GHz maser − − Leurini+in prep. − NOEMA observations • SiO(2-1) • 84.5 GHz maser ⇒ 3 outflows are detected, one associated with the maser 11 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018

Summary and future perspects • We selected 200 ATLASGAL clumps in different evolutionary phases of massive SF • We observed them in at least 4 masers (+ the 2 − J 1 -E lines in 60 sources) • Class I masers are detected in all phases also in the youngest 70µm-dark clumps ⇒ Most comprehensive catalogue of Class I masers: 1. are different masers associated with different evolutionary phases? 25 GHz series most only in bright IR sources 2. investigate shock structure with evolution ⇒ Ideal sample for follow-up interferometric studies to: 3. investigate star-formation activity in very early phases 4. investigate shock structure with evolution Acknowledgements: Effelsberg 100m telescope: T. Csengeri, K. König, A. Kraus, B. Winkel and all the telescope staff for helping/ performing the observations and solving calibration issues! Sardinia Radio Telescope: S. Casu, P. Castangia, A. Melis, A. Tarchi, A. Trois and all the INAF-OAC staff for helping my way into a new telescope! 12 The big impact of a big dish: Science with the Effelsberg 100-m Telescope, Bonn, 20-21 February 2018