Role of Public Participation in Denmark

Mizuno, Yoko; Yagishita, Masaharu; Wakuta, Yukihiro; Maeda, Hiroe; Zushiden, Satoko

doi:10.3392/sociotechnica.2.59

Cited by 4 publications

(3 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We used the 12 CO(J=1-0) and 12 CO(J=2-1) datasets obtained with NANTEN and NANTEN2. Observations of 12 CO(J=1-0) were carried out 1999 March to 2001 September by using the NANTEN telescope at Las Campanas in Chile with a positionswitching mode (Mizuno & Fukui 2004). The half-power beam width (HPBW) at 115 GHz, the grid spacing, and the velocity resolution are 2 .6, 2 , and 1 km s −1 , respectively.…”

Section: Molecular Line Observations With Nanten and Nanten2mentioning

confidence: 99%

Uniform Distribution of the Extremely Overionized Plasma Associated with the Supernova Remnant G359.1-0.5

Suzuki

Bamba

Enokiya

et al. 2020

ApJ

View full text Add to dashboard Cite

We report on the results of our detailed analyses on the peculiar recombining plasma of the supernova remnant (SNR) G359.1−0.5, and the interacting CO clouds. Combining Chandra and Suzaku data, we estimated the ionization state of the plasma with a careful treatment of the background spectrum. The average spectrum showed a remarkably large deviation of the electron temperature (∼0.17 keV) from the initial temperature (> 16 keV), indicating that the plasma is in a highly recombinationdominant state. On the other hand, the recombination timescale (n e t) is comparable to those of the other recombining SNRs (∼ 4.2 × 10 11 cm −3 s). We also searched for spatial variation of the plasma parameters, but found no significant differences.Using 12 CO(J=2-1) data obtained with NANTEN2, we found a new, plausible candidate for the interacting CO cloud, which has a line-of-sight velocity of ∼ −20 km s −1 . This indicates that the SNR is located at a distance of ∼4 kpc, which is the foreground of the Galactic center, as previously reported. The associated CO cloud does not show clear spatial coincidence with the nearby GeV/TeV emission, indicating that the origins of the GeV/TeV emission are likely unrelated to G359.1−0.5.

show abstract

Section: Molecular Line Observations With Nanten and Nanten2mentioning

confidence: 99%

Uniform Distribution of the Extremely Overionized Plasma Associated with the Supernova Remnant G359.1-0.5

Suzuki

Bamba

Enokiya

et al. 2020

ApJ

View full text Add to dashboard Cite

show abstract

“…Because M17 is bounded in longitude by potentially star-forming molecular clouds and in latitude by the Galactic mid-plane and the survey edge, there is no portion of the GLIMPSE image in Figure 1 that could be used as an off-source region to estimate the contamination in our sample from foreground or background sources (see §3.3). Fortunately, the region symmetric to M17, reflected above the Galactic mid-plane, lacks obvious CO emission marking molecular clouds (Sanders et al 1986;Mizuno & Fukui 2004) and is correspondingly free of the bright diffuse 8.0 µm emission in GLIMPSE that usually identifies H II regions. We selected a circular control field of 0.5 • radius centered at (l, b) = (15.08 • , 0.61 • ).…”

Section: Yso Selection and Characterizationmentioning

confidence: 99%

“…Jaffe & Fazio (1982) cast doubt on this sequential star formation scenario by presenting 13 farinfrared sources within the extended complex that did not show a progression of decreasing age with increasing distance from M17. Several high-resolution Galactic plane radio surveys in molecular or atomic line emission have included M17 (Sanders et al 1986;Mizuno & Fukui 2004;McClure-Griffiths et al 2005). The Massachusetts-Stony Brook Galactic Plane CO Survey (Sanders et al 1986), which provided (b, v) maps with 45 ′′ resolution that include M17 and its vicinity.…”

Section: Introductionmentioning

confidence: 99%

The Extended Environment of M17: A Star Formation History

Povich

Churchwell

Bieging

et al. 2009

ApJ

114

172

View full text Add to dashboard Cite

M17 is one of the youngest and most massive nearby star-formation regions in the Galaxy. It features a bright H II region erupting as a blister from the side of a giant molecular cloud (GMC). Combining photometry from the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) with complementary infrared (IR) surveys, we identify candidate young stellar objects (YSOs) throughout a 1.5 • × 1 • field that includes the M17 complex. The long sightline through the Galaxy behind M17 creates significant contamination in our YSO sample from unassociated sources with similar IR colors. Removing contaminants, we produce a highly-reliable catalog of 96 candidate YSOs with a high probability of association with the M17 complex. We fit model spectral energy distributions to these sources and constrain their physical properties. Extrapolating the mass function of 62 intermediate-mass YSOs (M ⋆ > 3 M ⊙ ), we estimate that >1000 stars are in the process of forming in the extended outer regions of M17. The remaining 34 candidate YSOs are found in a 0.17 deg 2 field containing the well-studied M17 H II region and photodissociation region, where bright diffuse mid-IR emission drastically reduces the sensitivity of the GLIMPSE point-source detections.By inspecting IR survey images from IRAS and GLIMPSE, we find that M17 lies on the rim of a large shell structure ∼0.5 • in diameter (∼20 pc at 2.1 kpc). We present maps of 12 CO and 13 CO (J = 2 → 1) emission observed with the Heinrich Hertz Telescope. The CO emission shows that the shell is a coherent, kinematic structure associated with M17, centered at v = 19 km s −1 . The shell is an extended bubble outlining the photodissociation region of a faint, diffuse H II region several Myr old. We identify a group of candidate ionizing stars within the bubble. YSOs in our catalog are concentrated around the bubble rim, providing evidence that massive star formation has been triggered by the expansion of the bubble. The formation of the massive cluster ionizing the M17 H II region itself may have been similarly triggered. We conclude that the star formation history in the extended environment of M17 has been punctuated by successive waves of massive star formation propagating through a GMC complex.

show abstract