scholarly journals The hidden heart of the luminous infrared galaxy IC 860

2019 ◽  
Vol 627 ◽  
pp. A147 ◽  
Author(s):  
S. Aalto ◽  
S. Muller ◽  
S. König ◽  
N. Falstad ◽  
J. Mangum ◽  
...  
Keyword(s):  
Velocity Gradient ◽  
Column Density ◽  
Rapid Evolution ◽  
Line Emission ◽  
Mass Function ◽  
Initial Mass Function ◽  
Continuum Emission ◽  
Vibrationally Excited ◽  
North East ◽  
The North

High-resolution (0.​​″03–0.​​″09 (9–26 pc)) ALMA (100–350 GHz (λ3 to 0.8 mm)) and (0.​​″04 (11 pc)) VLA 45 GHz measurements have been used to image continuum and spectral line emission from the inner (100 pc) region of the nearby infrared luminous galaxy IC 860. We detect compact (r ∼ 10 pc), luminous, 3 to 0.8 mm continuum emission in the core of IC 860, with brightness temperatures TB >  160 K. The 45 GHz continuum is equally compact but significantly fainter in flux. We suggest that the 3 to 0.8 mm continuum emerges from hot dust with radius r ∼ 8 pc and temperature Td ∼ 280 K, and that it is opaque at millimetre wavelengths, implying a very large H2 column density N(H2)≳1026 cm−2. Vibrationally excited lines of HCN ν2 = 1f J = 4 − 3 and 3–2 (HCN-VIB) are seen in emission and spatially resolved on scales of 40–50 pc. The line-to-continuum ratio drops towards the inner r = 4 pc, resulting in a ring-like morphology. This may be due to high opacities and matching HCN-VIB excitation- and continuum temperatures. The HCN-VIB emission reveals a north–south nuclear velocity gradient with projected rotation velocities of ν = 100 km s−1 at r = 10 pc. The brightest emission is oriented perpendicular to the velocity gradient, with a peak HCN-VIB 3–2 TB of 115 K (above the continuum). Vibrational ground-state lines of HCN 3–2 and 4–3, HC15N 4–3, HCO+ 3–2 and 4–3, and CS 7–6 show complex line absorption and emission features towards the dusty nucleus. Redshifted, reversed P-Cygni profiles are seen for HCN and HCO+ consistent with gas inflow with νin ≲ 50 km s−1. Foreground absorption structures outline the flow, and can be traced from the north-east into the nucleus. In contrast, CS 7–6 has blueshifted line profiles with line wings extending out to −180 km s−1. We suggest that a dense and slow outflow is hidden behind a foreground layer of obscuring, inflowing gas. The centre of IC 860 is in a phase of rapid evolution where an inflow is building up a massive nuclear column density of gas and dust that feeds star formation and/or AGN activity. The slow, dense outflow may be signaling the onset of feedback. The inner, r = 10 pc, IR luminosity may be powered by an AGN or a compact starburst, which then would likely require a top-heavy initial mass function.

scholarly journals High-velocity interstellar absorption associated with the supernova remnant W28

2020 ◽  
Vol 495 (3) ◽  
pp. 2909-2920 ◽  
Author(s):  
Adam M Ritchey
Keyword(s):  
High Velocity ◽  
Molecular Cloud ◽  
Supernova Remnant ◽  
Line Emission ◽  
Line Of Sight ◽  
Interstellar Gas ◽  
Lower Velocity ◽  
North East ◽  
The North ◽  
Visible Wavelengths

ABSTRACT We present an analysis of moderately high-resolution optical spectra obtained for the sightline to CD−23 13777, an O9 supergiant that probes high-velocity interstellar gas associated with the supernova remnant W28. Absorption components at both high positive and high negative velocity are seen in the interstellar Na i D and Ca ii H and K lines towards CD−23 13777. The high-velocity components exhibit low Na i/Ca ii ratios, suggesting efficient grain destruction by shock sputtering. High column densities of CH+, and high CH+/CH ratios, for the components seen at lower velocity may be indicative of enhanced turbulence in the clouds interacting with W28. The highest positive and negative velocities of the components seen in Na i and Ca ii absorption towards CD−23 13777 imply that the velocity of the blast wave associated with W28 is at least 150 km s−1, a value that is significantly higher than most previous estimates. The line of sight to CD−23 13777 passes very close to a well-known site of interaction between the supernova remnant and a molecular cloud to the north-east. The north-east molecular cloud exhibits broad molecular line emission, OH maser emission from numerous locations, and bright extended GeV and TeV γ-ray emission. The sightline to CD−23 13777 is thus a unique and valuable probe of the interaction between W28 and dense molecular gas in its environs. Future observations at ultraviolet and visible wavelengths will help to better constrain the abundances, kinematics, and physical conditions in the shocked and quiescent gas along this line of sight.

scholarly journals The rapid evolution of dust content in galaxies over the last five billion years

2012 ◽  
Vol 8 (S292) ◽  
pp. 275-278
Author(s):  
H. L. Gomez ◽  
L. Dunne ◽  
D. J. B. Smith ◽  
E. da Cunha
Keyword(s):  
Formation Rate ◽  
Rapid Evolution ◽  
Mass Function ◽  
Initial Mass Function ◽  
Stellar Atmospheres ◽  
Dust Content ◽  
Star Forming ◽  
First Time ◽  
Stellar Source ◽  
Science Demonstration

AbstractThe Herschel-ATLAS (H-ATLAS) will provide an unrivalled sample of galaxies, probing the normal star-forming submillimetre population of galaxies for the first time. Here, we exploit the Science Demonstration Phase (SDP) data to model the evolution of the interstellar content of galaxies in recent history. The most massive H-ATLAS galaxies show a large increase in the dust content five billion years ago compared to the present epoch. These observations are difficult to explain using standard dust models, one possibility could be contributions from a non-stellar source of dust e.g. grain growth in dense clouds; this would imply that less than 10% of dust would be condensed in stellar atmospheres. Alternatively, an initial mass function which becomes top heavy at high star formation rate densities could also explain this discrepancy.

scholarly journals A Molecular Disk Survey of Low-Mass Stars in the TW Hya Association

2015 ◽  
Vol 10 (S314) ◽  
pp. 207-208
Author(s):  
David R. Rodriguez ◽  
Gerrit van der Plas ◽  
Joel H. Kastner ◽  
Adam C. Schneider ◽  
Jacqueline K. Faherty ◽  
...  
Keyword(s):  
Line Emission ◽  
Mass Function ◽  
Continuum Emission ◽  
Molecular Gas ◽  
Low Mass Stars ◽  
Low Mass ◽  
Cold Dust

AbstractWe have carried out an ALMA Cycle 2 survey of 15 confirmed or candidate low-mass (<0.2M⊙) members of the TW Hya Association (TWA) with the goal of detecting line emission from CO molecular gas and continuum emission from cold dust. Our targets have spectral types of M4-L0 and hence represent the extreme low end of the TWA's mass function. The survey has yielded a detection of 12CO(2–1) emission around TWA 34. This newly discovered ~10 Myr-old molecular gas disk lies just ~50pc from Earth.

scholarly journals Dark supernova remnant

2020 ◽  
Vol 72 (6) ◽  
Author(s):  
Yoshiaki Sofue
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Rapid Evolution ◽  
Line Emission ◽  
Radio Continuum ◽  
Star Formation History ◽  
Continuum Emission ◽  
Round Hole ◽  
Formation History ◽  
The Galaxy

Abstract An almost perfect round hole of CO-line emission with a diameter of 3.7 pc was found in a molecular cloud (MC) centered on G35.75−0.25 (l = 35${{^{\circ}_{.}}}$75, b = −0${{^{\circ}_{.}}}$25) at radial velocity of 28 km s−1. The hole is quiet in radio continuum emission, unlike the usual supernova remnants (SNR), and the molecular edge is only weakly visible in 8 and 24 μm dust emissions. The hole may be either a fully evolved molecular bubble around a young stellar object (YSO), or a relic of a radio-quiet SNR that has already stopped expansion after rapid evolution in the dense MC as a buried SNR. Because G35.75 exhibits quite different properties from YSO-driven bubbles of the same size, we prefer the latter interpretation. The existence of such a “dark” SNR would affect the estimation of the supernova rate, and therefore the star formation history, in the Galaxy.

scholarly journals Vibrationally excited HC3N emission in NGC 1068: tracing the recent star formation in the starburst ring

2021 ◽  
Vol 502 (2) ◽  
pp. 3021-3034
Author(s):  
F Rico-Villas ◽  
J Martín-Pintado ◽  
E González-Alfonso ◽  
V M Rivilla ◽  
S Martín ◽  
...  
Keyword(s):  
Star Formation ◽  
Active Galactic Nucleus ◽  
Column Density ◽  
Local Thermodynamic Equilibrium ◽  
Continuum Emission ◽  
Vibrationally Excited ◽  
Star Forming ◽  
Dust Temperature ◽  
Ngc 1068 ◽  
The Continuum

ABSTRACT Using the ALMA data, we have studied the HC3N and continuum emission in the starburst pseudo-ring (SB pseudo-ring) and the circumnuclear disc (CND) of the SB/active galactic nucleus (AGN) composite galaxy NGC 1068. We have detected emission from vibrationally excited HC3N (HC3N*) only towards one star-forming region of the SB pseudo-ring. Remarkably, HC3N* was not detected towards the CND despite its large HC3N v = 0 column density. From local thermodynamic equilibrium (LTE) and non-LTE modelling of HC3N*, we obtained a dust temperature (Tdust) of ∼250 K and a density $(n_{\text{H}_2}) \text{ of }6\times 10^5$ cm−3 for this star-forming region. The estimated infrared (IR) luminosity of 5.8 × 108 L⊙ is typical of proto-superstar clusters (proto-SSCs) observed in the SB galaxy NGC 253. We use the continuum emissions at 147 and 350 GHz, along with CO and Pa α, to estimate the ages of other 14 SSCs in the SB pseudo-ring. We find the SSCs to be associated with the region connecting the nuclear bar with the SB pseudo-ring, supporting the inflow scenario. For the CND, our analysis yields Tdust ≤ 100 K and $n_{\text{H}_2}\sim (3\!-\!6)\times 10^5$ cm−3. The very different dust temperatures found for the CND and the proto-SSC indicate that, while the dust in the proto-SSC is being efficiently heated from the inside by the radiation from massive protostars, the CND is being heated externally by the AGN, which in the IR optically thin case can only heat the dust to 56 K. We discuss the implications of the non-detection of HC3N* near the luminous AGN in NGC 1068 on the interpretation of the HC3N* emission observed in the SB/AGN composite galaxies NGC 4418 and Arp 220.

scholarly journals Seeds of Life in Space (SOLIS)

2020 ◽  
Vol 637 ◽  
pp. A63 ◽  
Author(s):  
V. Taquet ◽  
C. Codella ◽  
M. De Simone ◽  
A. López-Sepulcre ◽  
J. E. Pineda ◽  
...  
Keyword(s):  
Column Density ◽  
Density Ratio ◽  
Sulfur Chemistry ◽  
Molecular Outflows ◽  
North East ◽  
The North ◽  
Chemical History ◽  
Low Mass ◽  
Chemical Conditions ◽  
Physical And Chemical

Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows. Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC 1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO2 towards NGC 1333-IRAS4A in the 1.3, 2, and 3 mm bands using the IRAM NOrthern Extended Millimeter Array and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east–south west direction. SO is detected at extremely high radial velocity up to + 25 km s−1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 105 cm−3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO2.

scholarly journals The physical and chemical structure of Sagittarius B2

2018 ◽  
Vol 614 ◽  
pp. A123 ◽  
Author(s):  
S. Pols ◽  
A. Schwörer ◽  
P. Schilke ◽  
A. Schmiedeke ◽  
Á. Sánchez-Monge ◽  
...  
Keyword(s):  
Radiative Transfer ◽  
Relative Abundance ◽  
Three Dimensional ◽  
Physical Structure ◽  
Continuum Emission ◽  
Gas Temperature ◽  
Vibrationally Excited ◽  
The North ◽  
Dust Temperature ◽  
Molecular Core

Context. We model the emission of methyl cyanide (CH3CN) lines towards the massive hot molecular core Sgr B2(M). Aims. We aim to reconstruct the CH3CN abundance field, and investigate the gas temperature distribution as well as the velocity field. Methods. Sgr B2(M) was observed with the Atacama Large Millimeter/submillimeter Array (ALMA) in a spectral line survey from 211 to 275 GHz. This frequency range includes several transitions of CH3CN (including isotopologues and vibrationally excited states). We employed the three-dimensional radiative transfer toolbox Pandora in order to retrieve the velocity and abundance field by modeling different CH3CN lines. For this purpose, we based our model on the results of a previous study that determined the physical structure of Sgr B2(M), i.e., the distribution of dust dense cores, ionized regions, and heating sources. Results. The morphology of the CH3CN emission can be reproduced by a molecular density field that consists of a superposition of cores with modified Plummer-like density profiles. The averaged relative abundance of CH3CN with respect to H2 ranges from 4 × 10−11 to 2 × 10−8 in the northern part of Sgr B2(M) and from 2 × 10−10 to 5 × 10−7 in the southern part. In general, we find that the relative abundance of CH3CN is lower at the center of the very dense, hot cores, causing the general morphology of the CH3CN emission to be shifted with respect to the dust continuum emission. The dust temperature calculated by the radiative transfer simulation based on the available luminosity reaches values up to 900 K. However, in some regions vibrationally excited transitions of CH3CN are underestimated by the model, indicating that the predicted gas temperature, which is assumed to be equal to the dust temperature, is partly underestimated. The determination of the velocity component along the line of sight reveals that a velocity gradient from the north to the south exists in Sgr B2(M).

scholarly journals ALMA resolves molecular clouds in metal-poor Magellanic Bridge A

2020 ◽  
Vol 641 ◽  
pp. A97 ◽  
Author(s):  
M. T. Valdivia-Mena ◽  
M. Rubio ◽  
A. D. Bolatto ◽  
H. P. Saldaño ◽  
C. Verdugo
Keyword(s):  
Star Formation ◽  
Molecular Clouds ◽  
Dust Emission ◽  
Line Emission ◽  
Far Infrared ◽  
Continuum Emission ◽  
Molecular Gas ◽  
The North ◽  
Mass Conversion ◽  
North And South

Context. The Magellanic Bridge is a tidal feature located between the Magellanic Clouds, containing young stars formed in situ. Its proximity allows high-resolution studies of molecular gas, dust, and star formation in a tidal low-metallicity environment. Aims. Our goal is to characterize gas and dust emission in Magellanic Bridge A, the source with the highest 870 μm excess of emission found in single-dish surveys. Methods. Using the ALMA telescope including the Morita Array, we mapped a 3′ field of view centered on the Magellanic Bridge A molecular cloud, in 1.3 mm continuum emission and 12CO(2−1) line emission at subparsec resolution. This region was also mapped in continuum at 870 μm and in 12CO(2−1) line emission at ~6 pc resolution with the APEX telescope. To study its dust properties, we also use archival Herschel and Spitzer data. We combine the ALMA and APEX 12CO(2−1) line cubes to study the molecular gas emission. Results. Magellanic Bridge A breaks up into two distinct molecular clouds in dust and 12CO(2−1) emission, which we call North and South. Dust emission in the North source, according to our best parameters from fitting the far-infrared fluxes, is ≈3 K colder than in the South source in correspondence to its less developed star formation. Both dust sources present large submillimeter excesses in LABOCA data: according to our best fits the excess over the modified blackbody (MBB) fit to the Spitzer/Herschel continuum is E(870 μm) ~ 7 and E(870 μm) ~ 3 for the North and South sources, respectively. Nonetheless, we do not detect the corresponding 1.3 mm continuum with ALMA. Our limits are compatible with the extrapolation of the MBB fits, and therefore we cannot independently confirm the excess at this longer wavelength. The 12CO(2−1) emission is concentrated in two parsec-sized clouds with virial masses of around 400 and 700 M⊙. Their bulk volume densities are n(H2) ~ 0.7−2.6 × 103 cm−3, higher than typical bulk densities of Galactic molecular clouds. The 12CO luminosity to H2 mass conversion factor αCO is 6.5 and 15.3 M⊙ (K km s−1 pc2)−1 for the North and South clouds, calculated using their respective virial masses and 12CO(2−1) luminosities. Gas mass estimates from our MBB fits to dust emission yields masses M ~ 1.3 × 103 M⊙ and 2.9 × 103 M⊙ for North and South, respectively, a factor of ~4 higher than the virial masses we infer from 12CO.

H76α Recombination Line Emission near Sgr A

1982 ◽  
Vol 4 (4) ◽  
pp. 453-454
Author(s):  
J. B. Whiteoak ◽  
F. F. Gardner
Keyword(s):  
Line Emission ◽  
Outer Edge ◽  
Recombination Line ◽  
Continuum Radiation ◽  
North East ◽  
The North ◽  
Sgr A

Our previous observations of the distribution of the H110α recombination line emission (rest frequency 4.87 GHz) towards Sgr A, obtained with the Parkes 64-m telescope and a 4′ .5 arc beam (Gardner and Whiteoak 1977 — to be referred to as Paper I), suggested that the emission was concentrated around the outer edge of the ‘arc’ of continuum radiation which extends 15′ arc to the north-east of the galactic nucleus.

The upper 2121 m at EastGRIP - Results from physical properties of NEGIS

2020 ◽  
Author(s):  
Nicolas Stoll ◽  
Ilka Weikusat ◽  
Johanna Kerch ◽  
Jan Eichler ◽  
Wataru Shigeyama ◽  
...  
Keyword(s):  
Grain Size ◽  
Ice Core ◽  
Rapid Evolution ◽  
Ice Cores ◽  
Flow Behaviour ◽  
Ice Streams ◽  
High Resolution Data ◽  
North East ◽  
The North ◽  
Ice Stream

&lt;div&gt; &lt;div&gt; &lt;div&gt; &lt;p&gt;Here we present the ice microstructure and CPO (c-axes fabric) data from the upper 2121 m of the EastGRIP ice core, an on-going deep drilling project on the North East Greenland Ice Stream. Understanding ice flow behaviour of fast flowing ice streams is crucial for accurate projections of future global sea level rise, but is still poorly understood due to e.g. missing observational fabric data from ice streams.&lt;/p&gt; &lt;p&gt;The presented CPO patterns found at EastGRIP show (1) a rapid evolution of c-axes anisotropy compared to deep ice cores from less dynamic sites, (2) a CPO evolution towards a strong vertical girdle and (3) CPO patterns that have not previously been directly observed in ice. Furthermore, data regarding grain properties (e.g. grain size) and indications of dynamic recrystallization, already at shallow depths, are presented.&lt;/p&gt; &lt;p&gt;The ice CPO shows a clear evolution with depth. In the first measurements at 111 m depth a broad single maximum distribution is observed, which transforms into a crossed girdle CPO (196-294 m). With increasing depth, an evolution towards a vertical girdle c-axes distribution occurs. Below 1150 m the CPO evolves into a vertical girdle with a higher density of c-axes oriented horizontally, a novel CPO in ice. These CPO patterns indicate a depth-related change in deformation modes, from vertical compression to extensional deformation along flow.&lt;/p&gt; &lt;p&gt;Grain size values are similar to results from other Greenlandic deep ice cores. Grain size evolution is characterized by an increase until 500 m depth, a decrease until 1360 m depth and mainly constant values in the Glacial. These findings are accompanied by indications of an early onset of dynamic recrystallisation e.g. irregular grain shapes, protruding grains and island grains.&lt;/p&gt; &lt;p&gt;The presented high-resolution data enable, for the very first time, a detailed and data- based look into a fast-flowing ice stream and are an important step towards a better understanding of the rheology of ice and its flow behaviour.&lt;/p&gt; &lt;/div&gt; &lt;/div&gt; &lt;/div&gt;

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