ASTE CO
                    <i>J</i>
                    = 3-2 SURVEY OF THE GALACTIC CENTER

Oka, Tomoharu; Onodera, Yui; Nagai, Makoto; Tanaka, K.; Matsumura, Shinji; Kamegai, Kazuhisa

doi:10.1088/0067-0049/201/2/14

Cited by 67 publications

(86 citation statements)

References 39 publications

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“…With only one pulsar, we cannot constrain the form or extent of the ionized gas from the pulsar observations. However, we can use observations of molecular gas (e.g., Oka et al 2012), radio thermal continuum emission (e.g., Law et al 2008), and radio recombination lines (Law et al 2009;Alves et al 2015) to establish a sufficiently reliable definition of the region as follows:…”

Section: Galactic Centermentioning

confidence: 99%

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Yao¹,

Manchester²,

Wang³

2017

ApJ

1,052

997

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We present a new model for the distribution of free electrons in the Galaxy, the Magellanic Clouds, and the intergalactic medium (IGM) that can be used to estimate distances to real or simulated pulsars and fast radio bursts (FRBs) based on their dispersion measure (DM). The Galactic model has an extended thick disk representing the so-called warm interstellar medium, a thin disk representing the Galactic molecular ring, spiral arms based on a recent fit to Galactic H II regions, a Galactic Center disk, and seven local features including the Gum Nebula, Galactic Loop I, and the Local Bubble. An offset of the Sun from the Galactic plane and a warp of the outer Galactic disk are included in the model. Parameters of the Galactic model are determined by fitting to 189 pulsars with independently determined distances and DMs. Simple models are used for the Magellanic Clouds and the IGM. Galactic model distances are within the uncertainty range for 86 of the 189 independently determined distances and within 20% of the nearest limit for a further 38 pulsars. We estimate that 95% of predicted Galactic pulsar distances will have a relative error of less than a factor of 0.9. The predictions of YMW16 are compared to those of the TC93 and NE2001 models showing that YMW16 performs significantly better on all measures. Timescales for pulse broadening due to interstellar scattering are estimated for (real or simulated) Galactic and Magellanic Cloud pulsars and FRBs.

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Section: Galactic Centermentioning

confidence: 99%

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Yao¹,

Manchester²,

Wang³

2017

ApJ

1,052

997

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“…The vast majority trace the neutral gas; these include the rotational transitions of CO isotopologues (e.g. Oka et al 1998Oka et al , 2011Oka et al , 2012Enokiya et al 2014), CS (Tsuboi et al 1999;Jones et al 2012), HCN (Jackson et al 1996;Jones et al 2012), N 2 H + (Jones et al 2012), H 2 CO (Ginsburg et al 2016), CH 3 CCH (Jones et al 2012), as well as NH 3 (Mills & Morris 2013) and OH (Yusef-Zadeh et al 1999), and the lower fine structure emission line of neutral carbon, [C i] (Martin et al 2004). However, these species do not trace major components of the inner Galaxy, where the gas is highly ionized or where the UV irradiated neutral gas is weakly ionized.…”

Section: Introductionmentioning

confidence: 99%

Kinematics and properties of the central molecular zone as probed with [C ii]

Langer

Velusamy

Morris³

et al. 2017

A&A

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Context. The Galactic Central Molecular Zone (CMZ) is a region containing massive and dense molecular clouds, with dynamics driven by a variety of energy sources including a massive black hole. It is thus the nearest template for understanding physical processes in extragalactic nuclei. The CMZ's neutral interstellar gas has been mapped spectrally in many neutral atomic and molecular gas tracers, but the ionized and CO-dark H 2 regions are less well traced spectroscopically. Aims. To identify features of the UV irradiated neutral gas, photon dominated regions (PDRs) and CO-dark H 2 , and highly ionized gas in the CMZ as traced by the fine structure line of C + at 158 µm, [C ii], and to characterize their properties. Methods. We observed the [C ii] 158 µm fine structure line with high spectral resolution using Herschel HIFI with two perpendicular On-the-Fly strip scans, along l = -0.• 8 to +0.• 8 and b = -0.• 8 to +0.• 8, both centered on (l,b) = (0We analyze the spatial-velocity distribution of the [C ii] data, compare them to those of [C i] and CO, and to dust continuum maps, in order to determine the properties and distribution of the ionized and neutral gas and its dynamics within the CMZ. Results. The longitude-and latitude-velocity maps of [C ii] trace portions of the orbiting open gas streams of dense molecular clouds, the cloud G0.253+0.016, also known as the Brick, the Arched Filaments, the ionized gas within several pc of Sgr A and Sgr B2, and the Warm Dust Bubble. We use the [C ii] data to determine the physical and dynamical properties of these CMZ features. Conclusions. The bright far-IR 158 µm C + line, [C ii], when observed with high spatial and spectral resolution, traces a wide range of emission features in the CMZ. The [C ii] emission arises primarily from dense PDRs and highly ionized gas, and is an important tracer of the kinematics and physical conditions of this gas.

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“…Maps of W3 and W5 (Bieging et al 2010;Bieging & Peters 2011) are also available. For the J = 3 → 2 line, the Galactic centre has been observed by Oka et al (2012), Orion by Ikeda et al (1999) and W3 by Bieging et al (2010). The ESA Planck satellite was launched on 14 May 2009 in order to (primarily) measure with unprecedented precision the temperature and polarization anisotropies of the cosmological microwave background (CMB).…”

Section: Introductionmentioning

confidence: 99%

Planck2013 results. XIII. Galactic CO emission

Ade

Aghanim

Alves

et al. 2014

A&A

159

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Rotational transition lines of CO play a major role in molecular radio astronomy as a mass tracer and in particular in the study of star formation and Galactic structure. Although a wealth of data exists for the Galactic plane and some well-known molecular clouds, there is no available high sensitivity all-sky survey of CO emission to date. Such all-sky surveys can be constructed using the Planck HFI data because the three lowest CO rotational transition lines at 115, 230 and 345 GHz significantly contribute to the signal of the 100, 217 and 353 GHz HFI channels, respectively. Two different component separation methods are used to extract the CO maps from Planck HFI data. The maps obtained are then compared to one another and to existing external CO surveys. From these quality checks the best CO maps, in terms of signal to noise ratio and/or residual contamination by other emission, are selected. Three different sets of velocity-integrated CO emission maps are produced with different trade-offs between signal-to-noise, angular resolution, and reliability. Maps for the CO J = 1 → 0, J = 2 → 1, and J = 3 → 2 rotational transitions are presented and described in detail. They are shown to be fully compatible with previous surveys of parts of the Galactic plane as well as with undersampled surveys of the high latitude sky. The Planck HFI velocity-integrated CO maps for the J = 1 → 0, J = 2 → 1, and J = 3 →2 rotational transitions provide an unprecedented all-sky CO view of the Galaxy. These maps are also of great interest to monitor potential CO contamination of the Planck studies of the cosmological microwave background.

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ASTE CO J = 3-2 SURVEY OF THE GALACTIC CENTER

Cited by 67 publications

References 39 publications

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Kinematics and properties of the central molecular zone as probed with [C ii]

Planck2013 results. XIII. Galactic CO emission

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