FIS Map Making Team

Yasuo Doi

Satoshi Takita, Takafumi Ootsubo, Masahiro Tanaka, Ko Arimatsu, Takahiro Morishima, Shinya Komugi, Norio Ikeda, Mitsunobu Kawada, Shuji Matsuura, Yoshimi Kitamura, Takao Nakagawa, Makoto Hattori, Elysandra F. Cypriano, Mireya Etxaluze, Glenn White

AKARI as a "super-IRAS"

• Improved spatial resolution
  • Down to \(\sim 1'\).
• Improved sensitivity
• Extended wavelength coverage \(>100\)\(\mu\)m
  • to cover Rayleigh-Jeans part of the dust emission

FIR All-Sky images

• Shorter wavebands \(\propto\) ISRF intensity
• Longer wavebands \(\propto\) ISRF intensity \(\times\) dust column

Dust Column Estimation

Improve accuracy/spatial resolution

• SFD : IRAS \(5'+\)T\(_{DIRBE}\)\(60'\)
• Planck(+SFD) : \(5'\)
• AKARI : \(\sim 1'\)

AKARI covers the peak of SED

Dust Column evaluation

Taurus region \(\tau\) map \((16^{\circ}\times12^{\circ})\)

AKARI can improve the spatial resolution of dust maps.

Spatial power spectra

Structure down to \(\sim2'\)(140\(\mu\)m) & \(\sim1'\)(90\(\mu\)m) can be successfully traced

(Polafis Flare region)

Omnipresence of ISM filaments

One of the key findings of Herschel

Filaments and star formation activities

"universal" \(\sim 0.1\)pc width of the filaments

\(>70\)% prestellar cores found in filaments

Filament formation – a 'missing link' in the star formation processes

From \(\sim100\)pc GMCs to \(<0.1\)pc prestellar cores

A giant leap in the spatical scale

http://www.astro.washington.edu/users/sjschmidt/A101/lectures.html

Necessity for the large spatial dynamic range in the observations

From \(>100\)pc GMCs to \(<0.1\)pc prestellar cores

\(>10^3\) difference in spatial scales

Obs. with high spatial resolution & spatially extended emission – "spatial dynamic range"

↓

Advantage of the AKARI All-sky Survey

Filament extraction @ PolarisFlare

Filament typical width: \(\sim 0.1\) pc \(\Leftrightarrow\) \(1.7'\) @ 200pc

Filament extraction @ PolarisFlare

Filament typical width: \(\sim 0.1\) pc \(\Leftrightarrow\) \(1.7'\) @ 200pc

Filament extraction @ Taurus

Filament typical width: \(\sim 0.1\) pc \(\Leftrightarrow\) \(2.5'\) @ 140pc

Filament extraction @ Taurus

Filament typical width: \(\sim 0.1\) pc \(\Leftrightarrow\) \(2.5'\) @ 140pc

Taurus YSOs

Filament typical width: \(\sim 0.1\) pc \(\Leftrightarrow\) \(2.5'\) @ 140pc

Taurus YSOs & TTSs correlation with filaments

YSOs: all sources (30/30)

TTSs: significant concentration (p-value=0.004)

\(\leftrightarrow\) 0.1[km/s] random motion over \(1-5\times10^6\) yrs

Summary

• AKARI data are now open to the public!!
• Multiple-waveband coverage at the peak of the dust SED
  • BGs color temperature, dust column evaluation
  • Dust composition, evolution
• Good spatial resolution, huge dynamic range
  • From global picture of diffuse ISM/giant molecular complex down to prestellar cores!!
  • Structure formation, phase transition, radiative transfer in denser regions, …

Release Announcement by ESA

Data Description Paper

Data Mirror Site