Integral field spectroscopy of Orion proplyds: metallicity and other properes

Yiannis Tsamis (ESO)

Nahiely Flores-Fajardo (UNAM Morelia/Beijing) Will Henney (UNAM Morelia) Adal Mesa-Delgado (Univ Chile) Daniel Pequignot (Meudon/Paris) Pepe Vilchez (IAA Granada) Jeremy Walsh (ESO) Proplyds in Orion

LV 2

• Adapted from Bally et al: HST WFPC2 (blue) + NICMOS (red: 2.15um cont + H2 line emission). H2 emission from slow C-type shocks 20-40 km/s (Colgan et al. 2007) The Orion Nebula proplyds

• The Sun was born in an Orion type cluster (Adams 2010) • Orion is distant (410 pc), but it contains massive hot stars capable of ionizing the proplyds. • Bright emission lines: plasma diagnoscs, metallicity probes.

HST Hα (Bally et al 2000) Coronal abundances of X-ray eming pre-main sequence Orion sources (Maggio et al. 2007)

S O Ar Ne

Fe • S, O, Ar, Ne Solar agree with B- stars and the Orion Nebula gas abundances

• Mg, Fe depleted compared to Solar and stellar values by up to ~few

Observaonal challenges: Keck HIRES long slit spectra of proplyds

• It is difficult to subtract the uneven nebular background and isolate the proplyd intrinsic emission with long slit methods

• Anomalous line profiles can be obtained: Henney & O’Dell (1999) background subtracon issues? The LV2 archetype - HST FOS single-aperture spectra

HST Hα+[NII] - OʼDell & Wen (1994) C2+ UV O+ C+

C = C+ + C2+ Optical O = O+ + O2+

θ1Ori C O2+ 3 circular HST FOS apertures (0.26”) within the 6.6”x4.2” VLT FLAMES/Argus IFU field (dashed box)

Tsamis et al. (2011), MNRAS, 412, 1367 Integral field spectroscopy of LV2 (VLT FLAMES/Argus IFU)

With IFU observations the background is still non-uniform but we have more room to move and to try and define it around a proplyd

Top left: O II 4649 recombination line – O2+ Top right: [O III] 5007 – O2+ Bottom left: [N II] 6584 – N+ Bottom right: [S II] 6731 – S+

Tsamis et al. (2011) Plasma physical condions: electron temperature and density

From observed line raos of temperature and density-sensive collisionally excited lines and comparing with theorecal raos

LV2 proplyd Temperature ~ 9000 K, Density ~ 106 cm-3

HST10 proplyd Temperature ~ 9000 K, Density ~ 3 x 104 cm-3

Abundance analysis based on collisionally excited lines (“forbidden lines”) [O III], [O II] , [N II], [S III] , [S II], [Ar III], [Ne III], etc. CII and OII recombinaon lines (RLs) from protoplanetary disks: novel metallicity diagnoscs

• This is the first detecon from proplyds: prominent in planetary nebulae and HII region spectra (e.g. Liu et al. 2000; Tsamis et al. 2003, 2008; Esteban et al. 2004, 2005).

• They are weak (<1% of Hbeta) but can be accurately measured in deep spectra.

• Atomic data for their analysis exists since the 1990s (Pequignot et al. 1991; Storey et al. 1994; Liu et al 1995; Davey et al. 2000; Storey in prep.)

• Abundances relave to H are a very weak funcon of temperature and density, hence, in principle, “bias-free”

VLT FLAMES/Argus (R~12000) Abundances in LV 2 vs. Orion HIIR vs. Sun

Proplyd Orion HIIR Sun (photosphere)

B-stars (Simon-Diaz’10) C = 8.35 N = 7.82 O = 8.74 Ne = 8.09

Tsamis et al. (2011)

• Super-solar values by factors of: C (x 2 – 3), O (x 2), Ne (x 2) • The Ne/S rao is > 2x Solar • Iron is 0.3% Solar (−2.5 dex) and 9% of the Orion gas value. Dust depleon similar to that seen towards cold ISM sightlines. àEvidence for grain growth? Iron in solids?

The jet of LV2 (VLT/FLAMES) (Tsamis & Walsh 2011)

• Spaally and spectrally resolving LV2’s bipolar jet (200 AU peak to peak)

• Fe/H (in jet lobe) ≥ 30-50% Solar Grains destroyed in shocks, iron is ejected into the gas phase Oxygen in the Universe HST 10 in Orion

[O I] 5577 emitted from the surface of the disc

Carbon recombination line

EUV/ FUV

photon Dynamic photoevaporation/photoionization Ionization models (based on Cloudy) used to front match the observations self-consistently:

Photoevaporation age ~ 104 yr, much shorter than age of Orion nebula, >105 yr: (i) Either the disc masses have been severely underestimated, or/and (ii) Discs were shielded from UV until recently (Tsamis et al. 2013) Results so far…

• HST 10 shows solar oxygen, and C, O, Ne that are practically the same as in B-type Orion stars. Fe is 0.2 dex lower than in M42 and 0.7 dex less than solar (empirical and model analysis – Tsamis et al 2013).

• LV2 shows elevated C, O, Ne compared to solar and to B-stars; Fe is 2.5 dex less than solar (empirical analysis, Tsamis et al 2011; Tsamis & Walsh 2011; models in preparation).

• HST 1 shows sub-solar O, and Fe 1.8 dex less than solar, but the analysis could not fully account for O+ as [O II] lines were not detected (empirical + model; Mesa-Delgado et al 2012).

• Sample is being enlarged with several other proplyds in Orion.

• VLT/SINFONI nIR IFU and X-shooter datasets under analysis/ construction