Radia%Ve Feedback from Massive Stars As Traced by Mul%Band Imaging and Spectroscopic Mosaics

Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Olivier Berne, Emilie Habart, Els Peeter

IRAP, Université Paul Saba:er, Toulouse, France IAS, Université Paris Sud, Orsay, France The University of Western Ontario, London, Canada

EWASS 2018

Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

PI team: Olivier Berné (France), Emilie Habart (France), Els Peeters (Canada)

CoIs: Abergel A. (Fr), Bergin E. (US), Bernard-Salas J. (UK), Bron E. (Sp), Cami J. (Ca), Cazaux S. (Nl), Dartois E. (Fr), Fuente A. (Sp), Goicoechea J. (Sp), Gordon K. (US), Okada Y. (Ge), Onaka T. (Jp), RoberZo M. (US), Röllig M. (Ge), Tielens A. (NL), Vicente S. (Pt), Wolﬁre M. (US)

120 Science collaborators from 18 countries. Team demographics:

Asia Australia 2 % Brasil CSA 8 % observers experimentalists 1 % 25 % women 42 % 46 % 31 % 57 % NASA ESA 75 % men 12 % modelers

www.jwst-ism.org Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics PI team: Olivier Berné (France), Emilie Habart (France), Els Peeters (Canada)

120 Science collaborators from 18 countries

Most of the energy massive stars inject in the the interstellar medium, is in the form of UV photons.

The far-UV (E<13.6 eV) photons are absorbed at the surface of molecular clouds, and re- emiLed in the infrared (IR). Such regions are called Photo-DissociaQon Regions.

A large fracQon of the IR emission in galaxies to be observed with JWST originates from PDRs

Understanding the physical and chemical processes at the origin of the extremely rich spectra of PDRs is a key objecQve for JWST.

Diﬀuse clouds, protoplanetary disk surfaces, irradiated globules, the envelopes of planetary nebulae, are also PDRs.

www.jwst-ism.org Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Photo-DissociaQon Regions

The scale length for FUV photon penetraQon corresponds to a few arcsec. JWST will resolve the transiQon from the molecular cloud to the PDR dissociaQon front, the ionizaQon front and the gas ﬂow into the ionized region

www.jwst-ism.org Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Choice of target for this program : Orion Bar

- Archetypical PDR - Nearby (414 pc) - Well studied - Completes GTO (Horsehead and NGC 7023) - Subject to change depending on date of launch : Triﬁd is the alterna9ve target - Total Qme ~30 hrs

HST (20x20’) Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

HSTHST (2.5x2.5’) Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

“Proplyds”

— 0.5’’

HSTHST (2.5x2.5’) Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

“Proplyds”

— 0.5’’

Proplyd

ALMA Globules Filaments

1’’ 0.002 HSTHST (2.5x2.5’) pc Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Current mul:wavelength view of the Orion Bar Halpha / HST PAH / VISIR 8 um HCO+ / ALMA

Ionized gaz at 1e4 K Neutral atomic gas at ~1e3 K HII region Molecular gas at few 10-100 K IonizaQon front

H/H2 dissociaQon front

Molecular cloud

15’’ Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Halpha / HST PAH / VISIR 8 um HCO+ / ALMA

Ionized gaz at 1e4 K Neutral atomic gas at ~1e3 K HII region NIRSPEC IFU mosaics 16.7 hours Molecular gas at few 10-100 K - Map over ~27x3” IonizaQon front - R~2700 - Angular resolu:on : 0.2’’ - Orders : short, medium long : 1-5.3 µm - MSA Leakcal for all observa:ons H/H2 dissociaQon front - Shown in overlay : region mapped by ALL wavelengths - Dedicated oﬀ observa:on

Molecular cloud

15’’ Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Halpha / HST PAH / VISIR 8 um HCO+ / ALMA

Ionized gaz at 1e4 K Neutral atomic gas at ~1e3 K HII region MIRI IFU mosaics (5.4 hours) Molecular gas at few 10-100 K IonizaQon front - Map over ~27x4” - R=1550-3250 - Angular resolu:on : 0.2’’ - Orders : short, medium long : 5-28 µm - Shown in overlay : region mapped by ALL H/H2 dissociaQon front wavelengths - Dedicated oﬀ observa:on

Molecular cloud

15’’ Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

JWST BeamSynthe:c spectra

5 μm 10 μm 25 μm

Figure 2: Model IR spectra of the 4 key regions within the interface of an H ii region around a massive star (or cluster) and the natal molecular cloud (Fig. 1) illustrating the spectral richness that JWST will observe. Dust scattered light and continuum emission are shown in dotted and dashed lines respectively. Ionic, atomic and molecular gas lines, PAHs and small dust bands are shown in colors. The bandpasses of the photometric ﬁlters selected in this ERS for lines and bands are shown in gray. Spectra have been calculated with the Meudon PDR code (7), Cloudy (8), DustEM (9) and PAHTAT (10).

atomic and H2 lines, all the known PAH bands, and dust emission features. Past observations of PDRs have been greatly hampered either by the limited spectral resolution which limits the detection of weak lines on a strong continuum, or by many telluric features which makes decomposition and accurate profile determinations of weak PAH subfeatures impossible. Indeed, PDR spectra are expected to be very rich and show a myriad of atomic and molecular lines which provide strong diagnostics of the physical conditions (Figs.2,4). The proposed observations will serve as a reference for accurate diagnostics of unresolved PDRs such as proto-planetary disk surfaces or distant star-forming regions. The proposed observations will produce “The JWST PDR template set” that will be used by a wide astronomical community to define their optimum JWST observing protocol to address a wide array of astronomical questions in which i) understanding the local physical conditions is a key scientific goal,

3 Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Halpha / HST PAH / VISIR 8 um HCO+ / ALMA

Ionized gaz at 1e4 K Neutral atomic gas at ~1e3 K HII region Molecular gas at few 10-100 K IonizaQon front MIRI Imaging + NIRCAM parallel (6.6 hours)

- 3x3 mosaic using subarray 128 H/H2 dissociaQon front - Angular resolu:on : 0.2’’ - Filters : 7.7 / 11.3 / 15 / 25.5 µm

Molecular cloud

15’’ Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

NIRCAM (1.4 hours)

- Full array in bright mode - 164N, 150W, 212N, 162M, 210 M - 405N, 444W, 335M, 410M, 300M Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Synthe'c)spectraSynthecc spectraSynthe:c spectra) a)a) HIIHII regionregion 1414 • 00 ++++ ++ ++++ ++++ ++++ Model(IR(spectra((R~3000)( 33 HH 1212 ArAr NeNe NeNe SS FeFe • Cloudy,(PDR(Meudon,(dustEM,(PAHTAT( Ionized gaz at 1e4 K 1010 • ObservaFons(NIRSPEC(IFU(+(NIRCAM(imaging( 2 8 Neutral atomic gas at ~1e3 K 2 8 • [FeII](1.64,(H2(2.12,(Br(α 4.05 + PAH(3.3(µm( 66 Molecular gas at few 10-100 K 11 44 ScatteredScattered lightlight 22 DustDust emissionemission 00 00 3030

b)b) IonizationIonization frontfront ++ 00 25 ++ ++ ++++ ++ ++ ++++ 66 FeFe HH 25 FeFe ArAr ArAr NeNe FeFe ArAr 2020 4 4 1515

1010 22 55 PAHsPAHs 00 00

c)c) PDR:PDR: HI/HHI/H dissociationdissociation frontfront 4040 22 ++ HH22 150150 HH22 FeFe

3030 100100 Flux (MJy/sr) Flux (MJy/sr) 2020

5050 1010 PAHsPAHs 00 00

1010 d)d) PDR:PDR: molecularmolecular zonezone 4040 HH22 HH22 HH22 88 3030 66 2020 44 1010 2 2 PAHsPAHs 00 00 11 22 33 44 55 55 66 77 88 99 1010 1515 2020 2525 11 μμmm 22 μμmm 55WavelengthWavelength μμmm ((µµm)m) ((((((((1(µm(((((((((((((((((((((((((((((((((((((((2(µm((((((((((((((((((((((((((((((((((((((((((((((((((5(µm( Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Synthe'c)spectraSynthecc spectra) Synthe:c spectra a) HII region 14 • 0 ++ + ++ ++ ++ Model(IR(spectra((R~3000)( 3 H 12 Ar Ne Ne S Fe • Cloudy,(PDR(Meudon,(dustEM,(PAHTAT( Ionized gaz at 1e4 K 10 • ObservaFons(MIRI(IFU(+(imaging( Neutral atomic gas at ~1e3 K 2 8 • PAH(7.7,(11.3(µm,(VSG(15(µm,(conFnuum(25.5(µm( 6 Molecular gas at few 10-100 K 1 4 Scattered light 2 Dust emission 0 0 30

b) Ionization front + 0 + + ++ + + ++ 6 Fe H 25 Fe Ar Ar Ne Fe Ar 20

4 15

10 2 5 PAHs 0 0

c) PDR: HI/H dissociation front 40 2 + H2 150 H2 Fe

30 100

Flux (MJy/sr) 20

50 10 PAHs 0 0

10 d) PDR: molecular zone 40 H2 H2 H2 8 30 6 20 4 10 2 PAHs 0 0 1 2 3 4 5 5 6 7 8 9 10 15 20 25 51 μ μmm 10 2 μ μmm 25 μ m 5Wavelength μm (µm) ((((((((5(µm((((((((((((((((((((((((((((((((((10(µm(((((((((((((((((((((((((((((((((((((((((((((((25(µm( Figure 2: Model IR spectra of the( 4 key regions within the interface of an H ii region around a massive star (or cluster) and the natal molecular cloud (Fig. 1) illustrating the spectral richness that JWST will observe. Dust scattered light and continuum emission are shown in dotted and dashed lines respectively. Ionic, atomic and molecular gas lines, PAHs and small dust bands are shown in colors. The bandpasses of the photometric ﬁlters selected in this ERS for lines and bands are shown in gray. Spectra have been calculated with the Meudon PDR code (7), Cloudy (8), DustEM (9) and PAHTAT (10).

3 Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Review of powerful NIR & MIR spectroscopic diagnostics

• Fine-structure lines of ions and atoms (IP<13.6 eV:[Fe II], [Fe I], [S II], [S I], [Ni II]..; IP>13.6 eV: [FeIII], [Ar III], [Ar II], [S IV], [SIII], [P III], [Ne III], [Ne II]..) [ionized gas before IF, IF-DF, inside PDRs; impinging EUV-FUV radiation field, cooling,

T, ne, pressure gradients → elemental abundances, metallicities (extragalactic need)] • Fluorescent lines (O, N..) [excelIent tracer of the IF front, intensity & wavelength dependence of the UV field] • Recombination lines (H, He, C..) [C+ layer at high resolution, physical conditions in the neutral layer beyond the IF]

• Pure rotational and rovibrational lines of H2 and possibly HD (both collisional & fluorescent) [major cooling, great thermometer for the bulk of the warm gas, pressure

gradients, H2 formation processes] + • Possibly high excited rotational & rovibrational lines of CO, H2O (HDO), OH, CH [hot gas / nonthermal processes, radiative & chemical formation pumping]

• Rovibrational lines of non-polar molecules (CH4, C2H2, HCN..) [complete inventory of hydrocarbon species, connection with grain processing] • Bands of carbonaceous dust it its multiforms (aromatic, aliphatic, fullerenes) • Continuum emission, dust scattering, extinction in the NIR Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Sub-features from aromacc/PAHs, aliphaccs, fullerenes .. Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Example of IR PDR diagnosccs

Excitacon diagrams from H2 lines observable by MIRI and NIRSpec as tracer of the warm and hot (UV pumped) excitacon temperatures (excitacon temperatures derived from the level populacons by a local Boltzmann ﬁt are indicated)

FeII lines as a tracer of the temperature and density distribucon from the ionized gas to the PDR

The 11.2/3.3 PAH raco as a tracer of PAH size Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

Science Enabling products in order to guide the preparaQon of Cycle 2 proposals on star-forming regions in our Galaxy and beyond

P1 : Enhanced data products

• Maps of integrated lines/bands from IFU spectroscopy cubes

• Template spectra (HII region, ID, DF, molecular zone) directly extracted from the observaQons or blind signal separaQon methods

P2 : Products facilita:ng data reduc:on and manipula:on

• Spectral order s:tching and s:tched cubes

• Cross-correlate spectra & images

• pyPAHFIT decompose the spectra into gas lines, dust MIRI Filters features (aromaQc/PAHs, aliphaQcs, fullerenes, silicates, ices), and dust conQnuum components (of all pixels in IFU maps)

• List of all the lines/bands present in the data Disentangling informaQon from ﬁlters requires spectroscopy Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

P3 : Data-interpreta:on tools

Using the PDR emission to trace the star formaQon into distant galaxies requires a precise understanding of the physical and chemical mechanisms that control the emission of the PDR

• H2 ﬁong tool maps of Tex, NH2 and Rotp

• PDR model toolbox web-based ﬁeng tool for maps to search in massive grids of complete models and derive physical parameters from observaQons of any number of lines

• PAHdb Spectral Analysis Tool decomposiQon of PAH ObservaQons ISM condiQons emission into contribuQng sub-populaQons (charge, size, composiQon, structure). Fit of the observaQons with theoreQcal/laboratory IR cross secQon spectra from the NASA Ames PAH IR Spectroscopic Database I H2(v=0,J=5->v=0,J=3)

• Ionized gas lines toolbox diagnosQc diagrams of key species for conversion of the lines intensiQes into physical condiQons

and exQncQon. Based on mulQ-level models or Cloudy ﬁeld radiation UV

Pressure These understanding can be transposed to a very wide range of environments: diﬀuse clouds, proto-planetary disk surfaces, envelope of planetary nebulae which are also PDRs! hLp://ismdb.obspm.fr + kosma-tau Radia%ve feedback from massive stars as traced by mul%band imaging and spectroscopic mosaics

www.jwst-ism.org

Community oriented program:

- Telecons open to the community will be organized on a regular basis - Community workshop - People interested are welcome to register on our website to keep posted and parQcipate

Take home message:

• A large frac:on of the IR emission in galaxies to be observed with JWST originates from PDRs (i.e. a largely neutral, but warm region of gas and dust FUV-irradiated)

• Understanding the physico-chemical processes at the origin of the extremely rich spectra of PDRs is a key objecQve for JWST

• The goal of this program is to obtain the ﬁrst spa:ally resolved, high spectral resolu:on observa:ons of a PDR well-deﬁned UV illuminaQon in a typical massive star-forming region using NIRCam, NIRSpec and MIRI

• Provide “template data” and science-enabling products for PDRs. Test used theoreQcal models and extend them into the JWST era

• Guide the preparaQon of Cycle 2 proposals on star-forming regions in our Galaxy and beyond