Where infall meets outflows: turbulent dissipation probed by CH+ and Lyα in the starburst/AGN galaxy group SMM J02399−0136 at <i>z</i> ∼ 2.8

Vidal-García, Alba; Falgarone, É.; Battaia, Fabrizio Arrigoni; Godard, B.; Ivison, R. J.; Herrera, Cinthya N.; Frayer, David; Andreani, P.; Li, Qiong; Gavazzi, R.

doi:10.1093/mnras/stab1503

Cited by 12 publications

(11 citation statements)

References 113 publications

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“…In one case the reservoir was found in proximity of the HzRG itself (Emonts et al 2016(Emonts et al , 2018, while in the second case around an Hα emitter (Dannerbauer et al 2017). Because of the similarities between the ELAN studied here and the halo expected to host an HzRG, and the high densities usually invoked to explain the Lyα emission, it is possible that ELANe are multiphasic, at least on tens of kiloparsec close to embedded sources (see also Vidal-García et al 2021). Interestingly, an extended molecular gas reservoir as massive as those found in HzRGs would increase the molecular gas budget for the targeted ELAN to values similar to the stars budget (see Figure 10).…”

Section: Note On Molecular Gas Extending Outside the Body Of Galaxiesmentioning

confidence: 68%

A Multiwavelength Study of ELAN Environments (AMUSE²). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

Battaia

Chen

Liu

et al. 2022

ApJ

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The systematic targeting of extended Lyα emission around high-redshift quasars resulted in the discovery of rare and bright Enormous Lyα Nebulae (ELANe) associated with multiple active galactic nuclei (AGNs). We initiate here “a multiwavelength study of ELAN environments” (AMUSE2) focusing on the ELAN around the z ∼ 3 quasar SDSS J1040+1020, aka the Fabulous ELAN. We report on VLT/HAWK-I, APEX/LABOCA, JCMT/SCUBA-2, SMA/850μm, and ALMA CO(5-4), and 2 mm observations and compare them to previously published VLT/MUSE data. The continuum and line detections enable a first estimate of the star formation rates, dust, stellar, and molecular gas masses in four objects associated with the ELAN (three AGNs and one Lyα emitter), confirming that the quasar host is the most star-forming (star formation rate of ∼500 M ⊙ yr−1) and massive galaxy (M star ∼ 1011 M ⊙) in the system, and thus can be assumed as central. All four embedded objects have similar molecular gas reservoirs ( M H 2 ∼ 10 10 M ⊙), resulting in short depletion timescales. This fact together with the estimated total dark matter halo mass, M DM = (0.8–2) × 1013 M ⊙, imply that this ELAN will evolve into a giant elliptical galaxy. Consistently, the constraint on the baryonic mass budget for the whole system indicates that the majority of baryons should reside in a massive warm/hot reservoir (up to 1012 M ⊙), needed to complete the baryons count. Additionally, we discuss signatures of gas infall on the compact objects as traced by Lyα radiative transfer effects and the evidence for the alignment between the satellites’ spins and their directions to the central.

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Section: Note On Molecular Gas Extending Outside the Body Of Galaxiesmentioning

confidence: 68%

A Multiwavelength Study of ELAN Environments (AMUSE²). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

Battaia

Chen

Liu

et al. 2022

ApJ

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“…This redshifted gas scatters photons back from the observer and contributes to the asymmetry of the Ly↵ line profiles. From these comparisons and a large set of multi-transition CO ancillary data [6], we conclude that the 20 kpc-scale CGM in SMM J02399−0136 is multi-phasic and inflowing towards the galaxies.…”

Section: What We Learn From the Comparison Of Ly↵ And Ch + Observationsmentioning

confidence: 88%

“…Finally, it has a high dipole moment, so absorption lines of its J=1-0 transition trace diffuse gas and emission lines trace high density gas seen in shocks and photodissociation regions [4,5]. All these properties make CH + a unique tracer of dissipation of mechanical energy in turbulence [3,6]. We have observed and detected the J=1-0 transition of CH + in 18 starburst galaxies at z'2-3.…”

Section: Introductionmentioning

confidence: 84%

“…1 and two reflection nebulae unseen in the sub-milimeter. The average redshift of the two galaxies, z ref = 2.8041 ± 0.0004, inferred from the ALMA CO(7-6) image at a resolution (0.48"⇥0.46"), is used as a reference for the velocity scale [6]. The spectra towards L2SW and L1 show broad lines of widths of ⇠600 and ⇠300 km s −1 respectively for CH + .…”

Section: Smm J02399-0136 Galaxy Groupmentioning

confidence: 99%

“…The absorption line against L2SW is redshifted by ⇠ 600 km s −1 , and therefore traces inflowing gas towards the galaxy. From the linewidth, we estimate the radius of the turbulent CGM to be ⇠20 kpc (see [6] for the details of the calculation), which corresponds to the integral scale of the CGM turbulence assuming that the width of the line is only due to turbulence. The line opacity provides the column density of CH + N(CH + ) ⇠ 6 ⇥ 10 14 cm −2 and from these observables we derive the mass of the turbulent CGM to be ⇠ 4 ⇥ 10 10 M � .…”

Section: Smm J02399-0136 Galaxy Groupmentioning

confidence: 99%

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CH⁺(1-0) in a z~2.8 galaxy group: Probe of multi-phasic turbulent gas reservoirs

Vidal-García

Falgarone²,

Battaia³

et al. 2022

EPJ Web of Conferences

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Starburst galaxies at redshifts z~2 to 4 are among the most intensely star-forming galaxies in the universe. The way they accrete their gas to form stars at such high rates is still a controversial issue. We have detected the CH+(1-0) line in emission and/or in absorption in all the gravitationally lensed starburst galaxies observed so far with ALMA in this redshift range. The unique spectroscopic and chemical properties of CH+ allow its rotational transition to highlight the sites of dissipation of mechanical energy. Whilst the absorption lines reveal highly turbulent reservoirs of low-density molecular gas extending far out of the galaxies, the broad emission lines with widths up to a few thousands of km/s, arise in myriad molecular shocks powered by the feedback of star formation and possibly active galactic nuclei. The CH+(1-0) lines therefore probe the sites of prodigious energy releases, mainly stored in turbulent reservoirs before being radiated away. These turbulent reservoirs act as extended buffers of mass and energy over timescales of a few tens to hundreds of Myr. Their mass supply involves multi-phasic gas inflows from galaxy mergers and/or cold stream accretion, as supported by Keck/KCWI Lyα observations of one of these starburst galaxies.

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Self-generated ultraviolet radiation in molecular shock waves

Lehmann

Godard

Forêts

et al. 2022

A&A

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Context. The energetics and physical conditions of the interstellar medium and feedback processes remain challenging to probe. Aims. Shocks, modelled over a broad range of parameters, are used to construct a new tool to deduce the mechanical energy and physical conditions from observed atomic or molecular emission lines. Methods. We compute magnetised, molecular shock models with velocities Vs = 5–80 km s−1, pre-shock proton densities nH = 102–106 cm−3, weak or moderate magnetic field strengths, and in the absence or presence of an external UV radiation field. These parameters represent the broadest published range of physical conditions for molecular shocks. As a key shock tracer, we focus on the production of CH+ and post-process the radiative transfer of its rovibrational lines. We develop a simple emission model of an ensemble of shocks for connecting any observed emission lines to the mechanical energy and physical conditions of the system. Results. For this range of parameters, we find the full diversity (C-, C*-, CJ-, and J-type) of magnetohydrodynamic shocks. H2 and H are dominant coolants, with up to 30% of the shock kinetic flux escaping in Lyα photons. The reformation of molecules in the cooling tail means H2 is even a good tracer of dissociative shocks and shocks that were initially fully atomic. The known shock tracer CH+ can also be a significant coolant, reprocessing up to 1% of the kinetic flux. Its production and excitation is intimately linked to the presence of H2 and C+. For each shock model we provide integrated intensities of rovibrational lines of H2, CO, and CH+, and atomic H lines, and atomic fine-structure and metastable lines. We demonstrate how to use these shock models to deduce the mechanical energy and physical conditions of extragalactic environments. As a template example, we interpret the CH+(1−0) emission from the Eyelash starburst galaxy. A mechanical energy injection rate of at least 1011 L⊙ into molecular shocks is required to reproduce the observed line. We find that shocks with velocities as low as 5 km s−1 irradiated by a strong UV field are compatible with the available energy budget. The low-velocity, externally irradiated shocks are at least an order magnitude more efficient than the most efficient shocks with no external irradiation in terms of the total mechanical energy required. We predict differences of more than two orders of magnitude in the intensities of the pure rotational lines of CO, Lyα, and the metastable lines of O, S+, and N between representative models of low-velocity (Vs ~ 10 km s−1) externally irradiated shocks and higher-velocity shocks (Vs ≥ 50 km s−1) with no external irradiation. Conclusions. Shock modelling over an extensive range of physical conditions allows for the interpretation of challenging observations of broad line emission from distant galaxies. Our new method opens up a promising avenue to quantitatively probe the physical conditions and mechanical energy of galaxy-scale gas flows.

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Where infall meets outflows: turbulent dissipation probed by CH+ and Lyα in the starburst/AGN galaxy group SMM J02399−0136 at z ∼ 2.8

Cited by 12 publications

References 113 publications

A Multiwavelength Study of ELAN Environments (AMUSE²). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

A Multiwavelength Study of ELAN Environments (AMUSE²). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

CH⁺(1-0) in a z~2.8 galaxy group: Probe of multi-phasic turbulent gas reservoirs

Self-generated ultraviolet radiation in molecular shock waves

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Where infall meets outflows: turbulent dissipation probed by CH+ and Lyα in the starburst/AGN galaxy group SMM J02399−0136 at z ∼ 2.8

Cited by 12 publications

References 113 publications

A Multiwavelength Study of ELAN Environments (AMUSE2). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

A Multiwavelength Study of ELAN Environments (AMUSE2). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

CH+(1-0) in a z~2.8 galaxy group: Probe of multi-phasic turbulent gas reservoirs

Self-generated ultraviolet radiation in molecular shock waves

Contact Info

Product

Resources

About

A Multiwavelength Study of ELAN Environments (AMUSE²). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

A Multiwavelength Study of ELAN Environments (AMUSE²). Mass Budget, Satellites Spin Alignment, and Gas Infall in a Massive z ∼ 3 Quasar Host Halo

CH⁺(1-0) in a z~2.8 galaxy group: Probe of multi-phasic turbulent gas reservoirs