Nario Kuno

University of Tsukuba

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Ming Zhu

Chinese Academy of Sciences

R. Plume

University of Calgary

Tie Liu

Shanghai Astronomical Observatory

Chenlin Zhou

Peng Cheng Laboratory

Hiroshi Matsuo

National Astronomical Observatory of Japan

Kee‐Tae Kim

Korea Astronomy and Space Science Institute

G. J. White

The Open University

Jinghua Yuan

National Astronomical Observatories

Christopher M. Brunt

University of Exeter

H. Thomas

Center for Astrophysics Harvard & Smithsonian

Cooperative Institutions

Chinese Academy of Sciences

National Astronomical Observatory of Japan

Max Planck Society

Institute of Astronomy and Astrophysics, Academia Sinica

Max Planck Institute for Radio Astronomy

Korea Astronomy and Space Science Institute

Centre National de la Recherche Scientifique

Purple Mountain Observatory

National Astronomical Observatories

Misato Observatory

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Sequential star formation in the filamentary structures of the Planck Galactic cold clump G181.84+0.31

Monthly Notices of the Royal Astronomical Society (2019)

Lixia Yuan Ming Zhu Tie Liu Jinghua Yuan Yuefang Wu

Abstract We present a multiwavelength study of the Planck Galactic cold clump G181.84+0.31, which is located at the northern end of the extended filamentary structure S242. We have extracted nine compact dense cores from the SCUBA-2 850-$\hbox{$\mu $m}$ map, and we have identified 18 young stellar objects (YSOs; four Class I and 14 Class II) based on their Spitzer, Wide-field Infrared Survey Explorer(WISE) and Two-Micron All-Sky Survey (2MASS) near- and mid-infrared colours. The dense cores and YSOs are mainly distributed along the filamentary structures of G181.84 and are well traced by HCO+(1–0) and N2H+(1–0) spectral-line emission. We find signatures of sequential star formation activities in G181.84: dense cores and YSOs located in the northern and southern substructures are younger than those in the central region. We also detect global velocity gradients of about 0.8 ± 0.05 and 1.0 ± 0.05 km s−1 pc−1 along the northern and southern substructures, respectively, and local velocity gradients of 1.2 ± 0.1 km s−1 pc−1 in the central substructure. These results might be due to the fact that the global collapse of the extended filamentary structure S242 is driven by an edge effect, for which the filament edges collapse first and then further trigger star formation activities inward. We identify three substructures in G181.84 and estimate their critical masses per unit length, which are ∼101 ± 15, 56 ± 8 and 28 ± 4 M⊙ pc−1, respectively. These values are all lower than the observed values (∼200 M⊙ pc−1), suggesting that these substructures are gravitationally unstable.

Young stellar object

Substructure

Line (geometry)

Galactic plane

10.1093/mnras/stz1266

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Citations (4)

<title>Flight performance of submillimeter-wave telescope on board S-520-17</title>

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (1995)

Hiroshi Matsuo Junji Inatani Nario Kuno Keisuke Miyazawa Kenichi Okumura

Submillimeter-wave telescope on board S-520-17 was launched on January 23, 1995. The telescope is dedicated for observation of cold dust within Orion molecular cloud. In this paper, a brief description of the telescope system and review through the environmental test, preflight calibration, and flight performance is described. Also discussed in the last section is a development of array detectors for future space mission in far-infrared and submillimeter- wave.

Submillimeter wave

Spitzer Space Telescope

On board

Infrared telescope

10.1117/12.221386

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On the absence of molecular absorption in high-redshift millimetre-band searches

Monthly Notices of the Royal Astronomical Society (2011)

S. J. Curran M. T. Whiting F. Combes Nario Kuno Paul Francis

We have undertaken a search for millimetre-wave band absorption (through the CO and HCO+ rotational transitions) in the host galaxies of reddened radio sources (z = 0.405-1.802). Despite the colour selection (optical-near infrared colours of V - K > 5 in all but one source), no absorption was found in any of the eight quasars for which the background continuum flux was detected. On the basis of the previous (mostly intervening) H2 and OH detections, the limits reached here and in some previous surveys should be deep enough to detect molecular absorption according to their V - K colours. However, our survey makes the assumption that the reddening is associated with dust close to the emission redshift of the quasar and that the narrow millimetre component of this emission is intercepted by the compact molecular cores. By using the known millimetre absorbers to define the colour depth and comparing this with the ultra-violet luminosities of the sources, we find that, even if these assumptions are valid, only twelve of the forty objects (mainly from this work) are potentially detectable. This is assuming an excitation temperature of 10 K at z=0, with the number decreasing with increasing temperatures (to zero detectable at 100 K).

Molecular absorption

Ultraviolet

Excitation temperature

10.1111/j.1365-2966.2011.19193.x

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Citations (23)

Millimeter-wave continuum observation of high-z radio quasars

Advances in Space Research (1999)

Hiroshi Matsuo Nario Kuno H. Kashihara G. S. Tsarevsky

Extremely high frequency

10.1016/s0273-1177(99)00249-5

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The interstellar medium in Andromeda's dwarf spheroidal galaxies – II. Multiphase gas content and ISM conditions

Monthly Notices of the Royal Astronomical Society (2016)

I. De Looze M. Baes D. Cormier Hiroyuki Kaneko Nario Kuno

We make an inventory of the interstellar medium material in three low-metallicity dwarf spheroidal galaxies of the Local Group (NGC147, NGC185 and NGC205). Ancillary HI, CO, Spitzer IRS spectra, H{\alpha} and X-ray observations are combined to trace the atomic, cold and warm molecular, ionised and hot gas phases. We present new Nobeyama CO(1-0) observations and Herschel SPIRE FTS [CI] observations of NGC205 to revise its molecular gas content. We derive total gas masses of M_gas = 1.9-5.5x10^5 Msun for NGC185 and M_gas = 8.6-25.0x10^5 Msun for NGC205. Non-detections combine to an upper limit on the gas mass of M_gas =< 0.3-2.2x10^5 Msun for NGC147. The observed gas reservoirs are significantly lower compared to the expected gas masses based on a simple closed-box model that accounts for the gas mass returned by planetary nebulae and supernovae. The gas-to-dust mass ratios GDR~37-107 and GDR~48-139 are also considerably lower compared to the expected GDR~370 and GDR~520 for the low metal abundances in NGC 185 (0.36 Zsun) and NGC205 (0.25 Zsun), respectively. To simultaneously account for the gas deficiency and low gas-to-dust ratios, we require an efficient removal of a large gas fraction and a longer dust survival time (~1.6 Gyr). We believe that efficient galactic winds (combined with heating of gas to sufficiently high temperatures in order for it to escape from the galaxy) and/or environmental interactions with neighbouring galaxies are responsible for the gas removal from NGC147, NGC185 and NGC205.

Andromeda

10.1093/mnras/stw3001

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CHIMPS2: survey description and 12CO emission in the Galactic Centre

Monthly Notices of the Royal Astronomical Society (2020)

David Eden T. J. T. Moore M. J. Currie A. J. Rigby Erik Rosolowsky

The latest generation of Galactic-plane surveys is enhancing our ability to study the effects of galactic environment upon the process of star formation. We present the first data from CO Heterodyne Inner Milky Way Plane Survey 2 (CHIMPS2). CHIMPS2 is a survey that will observe the Inner Galaxy, the Central Molecular Zone (CMZ), and a section of the Outer Galaxy in $^{12}$CO, $^{13}$CO, and C$^{18}$O $(J = 3\rightarrow2)$ emission with the Heterodyne Array Receiver Program on the James Clerk Maxwell Telescope (JCMT). The first CHIMPS2 data presented here are a first look towards the CMZ in $^{12}$CO J = 3$\rightarrow$2 and cover $-3^{\circ}\leq\,\ell\,\leq\,5^{\circ}$ and $\mid$b$\mid \leq 0.5^{\circ}$ with angular resolution of 15 arcsec, velocity resolution of 1 km s$^{-1}$, and rms $\Delta T_A ^\ast =$ 0.58 K at these resolutions. Such high-resolution observations of the CMZ will be a valuable data set for future studies, whilst complementing the existing Galactic Plane surveys, such as SEDIGISM, the Herschel infrared Galactic Plane Survey, and ATLASGAL. In this paper, we discuss the survey plan, the current observations and data, as well as presenting position-position maps of the region. The position-velocity maps detect foreground spiral arms in both absorption and emission.

Galactic plane

10.1093/mnras/staa2734

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Citations (28)

CHIMPS: the¹³CO/C¹⁸O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey

Monthly Notices of the Royal Astronomical Society (2015)

A. J. Rigby T. J. T. Moore R. Plume David Eden J. S. Urquhart

We present the $^{13}$CO/C$^{18}$O (J=3-2) Heterodyne Inner Milky Way Plane Survey (CHIMPS) which has been carried out using the Heterodyne Array Receiver Program on the 15 m James Clerk Maxwell Telescope (JCMT) in Hawaii. The high-resolution spectral survey currently covers |b| < 0.5 deg and 28 < l < 46 deg, with an angular resolution of 15 arcsec in 0.5 km/s velocity channels. The spectra have a median rms of $\sim$ 0.6 K at this resolution, and for optically thin gas at an excitation temperature of 10 K, this sensitivity corresponds to column densities of $N_{\mathrm{H}_{2}} \sim 3 \times 10^{20}\,$cm$^{-2}$ and $N_{\mathrm{H}_{2}} \sim 4 \times 10^{21}\,$cm$^{-2}$ for $^{13}$CO and C$^{18}$O, respectively. The molecular gas that CHIMPS traces is at higher column densities and is also more optically thin than in other publicly available CO surveys due to its rarer isotopologues, and thus more representative of the three-dimensional structure of the clouds. The critical density of the J=3-2 transition of CO is $\gtrsim 10^{4}$ cm$^{-3}$ at temperatures of $\leq 20$ K, and so the higher density gas associated with star formation is well traced. These data complement other existing Galactic plane surveys, especially the JCMT Galactic Plane Survey which has similar spatial resolution and column density sensitivity, and the Herschel infrared Galactic Plane Survey. In this paper, we discuss the observations, data reduction and characteristics of the survey, presenting integrated emission maps for the region covered. Position-velocity diagrams allow comparison with Galactic structure models of the Milky Way, and while we find good agreement with a particular four arm model, there are some significant deviations.

Galactic plane

Isotopologue

Spectral resolution

10.1093/mnras/stv2808

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Citations (94)

Refined molecular gas mass and star-formation efficiency in NGC 3627

Monthly Notices of the Royal Astronomical Society (2011)

Yoshimasa Watanabe Kazuo Sorai Nario Kuno A. Habe

We present a 13CO (J= 1–0) mapping observation of the nearby barred spiral galaxy NGC 3627, covering almost all the stellar disc, with the Nobeyama 45-m telescope. We found that the 13CO (J= 1–0) morphology of NGC 3627 is similar to the 12CO (J= 1–0) map and the 12CO (J= 1–0)/13CO (J= 1–0) intensity ratio is 10.7 ± 0.4 on average. We also found that the ratio varies position-to-position in the galaxy and decreases with the galactocentric distance. The ratio is especially high, ∼20, in the bar and this result suggests that the molecular gas mass calculated from the 12CO (J= 1–0) intensity with constant conversion factor is overestimated in the bar. As a result, the star-formation efficiency (SFE) in the bar, which is derived from 13CO (J= 1–0) intensity, is similar to that in the other regions except for the two bar ends and the centre. We found that the SFE is higher in the bar ends than in the other regions. We discuss plausible reasons for the enhanced SFE in the bar: the kinetic temperature of the molecular gas, the spatial gap between the molecular gas peak and star formation and gravitational instability.

Bar (unit)

Intensity

Star (game theory)

Gravitational potential

Mean kinetic temperature

Barred spiral galaxy

10.1111/j.1365-2966.2010.17746.x

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Citations (38)

A multiwavelength analysis of the clumpy FIR-bright sources in M33

Monthly Notices of the Royal Astronomical Society (2014)

Giovanni Natale K. Foyle C. D. Wilson Nario Kuno

We present a multiwavelength study of a sample of far-infrared (FIR) sources detected on the Herschel broad-band maps of the nearby galaxy M33. We perform source photometry on the FIR maps as well as mid-infrared (MIR), Hα, far-ultraviolet and integrated H i and CO line emission maps. By fitting MIR/FIR dust emission spectra, the source dust masses, temperatures and luminosities are inferred. The sources are classified based on their Hα morphology (sub-structured versus not-substructured) and on whether they have a significant CO detection (S/N > 3σ). We find that the sources have dust masses in the range 102–104 M⊙ and that they present significant differences in their inferred dust/star formation/gas parameters depending on their Hα morphology and CO detection classification. The results suggests differences in the evolutionary states or in the number of embedded H ii regions between the sub-samples. The source background-subtracted dust emission seems to be predominantly powered by local star formation, as indicated by a strong correlation between the dust luminosity and the dust-corrected Hα luminosity and the fact that the extrapolated young stellar luminosity is high enough to account for the observed dust emission. Finally, we do not find a strong correlation between the dust-corrected Hα luminosity and the dust mass of the sources, consistent with previous results on the breakdown of simple scaling relations at sub-kpc scales. However, the scatter in the relation is significantly reduced by correcting the Hα luminosity for the age of the young stellar populations in the star-forming regions.

10.1093/mnras/stu560

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Gas velocity patterns in simulated galaxies: observational diagnostics of spiral structure theories

Monthly Notices of the Royal Astronomical Society (2016)

Junichi Baba Kana Morokuma-Matsui Yusuke Miyamoto Fumi Egusa Nario Kuno

There are two theories of stellar spiral arms in isolated disc galaxies that model stellar spiral arms with different longevities: quasi-stationary density wave theory, which characterizes spirals as rigidly rotating, long-lived patterns (i.e. steady spirals), and dynamic spiral theory, which characterizes spirals as differentially rotating, transient, recurrent patterns (i.e. dynamic spirals). In order to discriminate between these two spiral models observationally, we investigated the differences between the gas velocity patterns predicted by these two spiral models in hydrodynamic simulations. We found that the azimuthal phases of the velocity patterns relative to the gas density peaks (i.e. gaseous arms) differ between the two models, as do the gas flows; nevertheless, the velocity patterns themselves are similar for both models. Such similarity suggests that the mere existence of streaming motions does not conclusively confirm the steady spiral model. However, we found that the steady spiral model shows that the gaseous arms have radial streaming motions well inside the co-rotation radius, whereas the dynamic spiral model predicts that the gaseous arms tend to have tangential streaming motions. These differences suggest that the gas velocity patterns around spiral arms will enable distinction between the spiral theories.

Barred spiral galaxy

Density wave theory

Irregular galaxy

Unbarred spiral galaxy

10.1093/mnras/stw987

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Citations (29)