HST/WFC3 imaging of protostellar jets in Carina: [Fe II] emission tracing massive jets from intermediate-mass protostars

Reiter, Megan; Smith, Nathan

doi:10.1093/mnras/stt889

Cited by 30 publications

(93 citation statements)

References 68 publications

(95 reference statements)

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“…However, given the uncertainties on the mass estimation for the disks (a factor of 3 or 4), it could also be possible that the star in the middle is an intermediate-mass star. This is in agreement with recent observations (Reiter & Smith 2013.…”

Section: Hh 901supporting

confidence: 94%

ALMA Observations of the Extraordinary Carina Pillars: HH 901/902

Cortes-Rangel¹,

Zapata²,

Toalá³

et al. 2020

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We present Atacama Large Millimeter/Submillimeter Array (ALMA) 1.3 mm continuum and C 18 O(2−1), N 2 D + (3−2), 13 CS(5−4), and 12 CO(2−1) line sensitive and high angular resolution (∼0.3 ) observations of the famous carina pillars and protostellar objects HH 901/902. Our observations reveal for the first time, the bipolar CO outflows and the dusty disks (plus envelopes) that are energizing the extended and irradiated HH objects far from the pillars. We find that the masses of the disks+envelopes are about 0.1 M and of the bipolar outflows are between 10 −3 -10 −4 M , which suggests that they could be low-or maybe intermediate-mass protostars. Moreover, we suggest that these young low-mass stars are likely embedded Class 0/I protostars with high-accretion rates. We also show the kinematics of the gas in the pillars together with their respective gas masses (0.1 -0.2 M ). We estimate that the pillars will be photo-evaporated in 10 4 to 10 5 years by the massive and luminous stars located in the Trumpler 14 cluster. Finally, given the short photo-evaporated timescales and that the protostars in these pillars are still very embedded, we suggest that the disks inside of the pillars will be quickly affected by the radiation of the massive stars, forming proplyds, like those observed in Orion.

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Section: Hh 901supporting

confidence: 94%

ALMA Observations of the Extraordinary Carina Pillars: HH 901/902

Cortes-Rangel¹,

Zapata²,

Toalá³

et al. 2020

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“…This rate should be treated as a lower limit, since there can be more IFOs simply undetected due to the limit in imaging depth and imaging resolution. For instance, the HST -ACS data shows a higher detection rate of HH objects against the YSOs, 21/444 = 4.7 % (Smith et al 2010a;Povich et al 2011b;Reiter & Smith 2013). As far as we know, our study is the first, unbiased, wide-field [Fe II] 1.64 µm imaging observation of jets and outflows from YSOs in the massive star forming region, where YSO's evolutionary stages are determined.…”

Section: Detection Rate Of [Fe Ii] Featuresmentioning

confidence: 78%

“…In this section, we estimate the detection rate of IFOs in relation with this information. 23 HH objects and 16 HH candidates were identified over several selected regions of the Carina Nebula, using ground and space telescopes (Smith et al 2004(Smith et al , 2010aReiter & Smith 2013). Among them, 10 HH objects and 5 HH candidates, including HHc-16 identified by ourselves, fall within our observation field (cf.…”

Section: Detection Rate Of [Fe Ii] Featuresmentioning

confidence: 99%

“…If A Hα = 2.54 mentioned above is applied,Ṁ out from Hα data is increased by about a factor of three, sinceṀ out is proportional to the square-root of Hα intensity in the estimation of Smith et al (2010a). The neutral gas excluded in the Hα estimation is another reason for the differentṀ out (Reiter & Smith 2013). For IFO-1 and -2, the different dynamical time, τ , used in section 3.2.2 could account for the difference, because the [Fe II] feature used for theṀ out estimation is farther from the jet-driving object than the Hα feature used for theṀ out estimation (Fig.…”

Section: Four Ifos and Their Corresponding Hh Objectsmentioning

confidence: 99%

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[Fe II] 1.64 μm FEATURES OF JETS AND OUTFLOWS FROM YOUNG STELLAR OBJECTS IN THE CARINA NEBULA

Shinn¹,

Pyo²,

Lee³

et al. 2013

ApJ

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We present [Fe II] 1.64 µm imaging observations for jets and outflows from young stellar objects (YSOs) over the northern part (∼ 24 × 45 ) of the Carina Nebula, a massive star forming region. The observations were performed with IRIS2 of Anglo-Australian Telescope and the seeing was ∼ 1.5 ± 0.5 . Eleven jet and outflow features are detected at eight different regions, and are named as Ionized Fe Objects (IFOs). One Herbig-Haro object candidate missed in Hubble Space Telescope Hα observations is newly identified as HHc-16, referring our [Fe II] images. IFOs have knotty or longish shapes, and the detection rate of IFOs against previously identified YSOs is 1.4 %, which should be treated as a lower limit. Four IFOs show an anti-correlated peak intensities in [Fe II] and Hα, where the ratio I([Fe II])/I(Hα) is higher for longish IFOs than for knotty IFOs. We estimate the outflow mass loss rate from the [Fe II] flux, using two different methods. The jet-driving objects are identified for three IFOs (IFO-2, -4, and -7), for which we study the relations between the outflow mass loss rate and the

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“…Although observations suggest outflows may have little effect on the largest scale turbulence in molecular clouds (e.g. Mac Low & Klessen 2004;Padoan et al 2009;Zrake & MacFadyen 2012;Reiter & Smith 2013), the compressive modes they generate may still be important at triggering star formation on small scales (Schneider et al 2011). …”

Section: Introductionmentioning

confidence: 99%

Power spectra of outflow-driven turbulence

Moraghan¹,

Kim²,

Yoon³

2015

Monthly Notices of the Royal Astronomical Society

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We investigate the power spectra of outflow-driven turbulence through high-resolution three-dimensional isothermal numerical simulations where the turbulence is driven locally in real-space by a simple spherical outflow model. The resulting turbulent flow saturates at an average Mach number of ∼ 2.5 and is analysed through density and velocity power spectra, including an investigation of the evolution of the solenoidal and compressional components. We obtain a shallow density power spectrum with a slope of ∼ −1.2 attributed to the presence of a network of localised dense filamentary structures formed by strong shock interactions. The total velocity power spectrum slope is found to be ∼ −2.0, representative of Burgers shock dominated turbulence model. The density weighted velocity power spectrum slope is measured as ∼ −1.6, slightly less than the expected Kolmogorov scaling value (slope of -5/3) found in previous works. The discrepancy may be caused by the nature of our real space driving model and we suggest there is no universal scaling law for supersonic compressible turbulence. We find that on average, solenoidal modes slightly dominate in our turbulence model as the interaction between strong curved compressible shocks generates solenoidal modes, and compressible modes decay faster.

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HST/WFC3 imaging of protostellar jets in Carina: [Fe II] emission tracing massive jets from intermediate-mass protostars

Cited by 30 publications

References 68 publications

ALMA Observations of the Extraordinary Carina Pillars: HH 901/902

ALMA Observations of the Extraordinary Carina Pillars: HH 901/902

[Fe II] 1.64 μm FEATURES OF JETS AND OUTFLOWS FROM YOUNG STELLAR OBJECTS IN THE CARINA NEBULA

Power spectra of outflow-driven turbulence

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