ASTRO-F

Large-Scale Surveys&
Mission Programs

2005/09/12
ASTRO-F Program Committee

List of Large-Area Surveys (LS) and Mission Programs (MP)
ID

Title

Contact Person

Planned No. of Pointings

LSASS

All-Sky Survey

H. Shibai

N/A

LSNEP

North Ecliptic Pole (NEP) Survey

H. Matsuhara

954

LSLMC

Large Magellanic Cloud (LMC) Survey

T. Onaka866

LS Subtotal
ID

1820

Title

Principal
Investigator

Approved Numberof Pointhings
Priority Priority Priority
A
B
A+B

AFSAS

ASTRO-F Studies on Star Formation and M. Ueno
Star Forming Regions

400

400

800

AGBGA

Mass Loss and Stellar Evolution in the AGB Y. Nakada
phase

112

112

224

AGNUL

Evolution of ULIRGs and AGNs

T. Nakagawa

50

50

100

CLEVL

Evolution of Clusters of Galaxies

H.-M. Lee

173

173

346

CNIRB

ASTRO-F
ObservationsofCosmic S. Matsuura
Near-Infrared Background Radiation

0

0

0

FBSEP

ASTRO-F
ObservationsofCosmic S. Matsuura
Far-Infrared Background Radiation andDistant Infrared Galaxies in Low-Cirrus
Region near South Ecliptic Pole

270

0

270

FISS3

FIS Serendipitous Spectroscopic Survey

M. Kawada

0

0

0

FUHYU

Spitzer Well Studied Field Mission Program

C.Pearson

25

25

50

GALEV

Dusty Star-Formation
Universe

the H. Matsuhara

40

26

66

ISMGN

Interstellar Dust and Gas in Various H. Kaneda
Environments of our Galaxy and Nearby
Galaxies

250

242

492

MLHES

Excavating Mass Loss History in Extended I. Yamamura
Dust Shells of Evolved Stars

100

100

200

NIRLT

Near Infrared Spectroscopy of L and T I. Yamamura
Dwarfs

25

25

50

SOSOS

Origin and Evolution of Solar System M. Ueno
Objects

176

178

354

SPICY

Unbiased Slit-less Spectroscopic Survey of T. Wada
Galaxies

100

100

200

VEGAD

Debris Disks around Main Sequence Stars H. Murakami
and Extra-solar Zodiacal Emissions

216

216

432

1924

1639

3584

Historyof

MP Subtotal
Total

5404

ASTRO-F Large-Scale Survey Program
Title (Abbreviation)
Title (Full)Contact Person

Date: 05/08/12

LSASS
The ASTRO-F All-Sky Survey
Shibai, Hiroshi

E-mail: shibai@nagoya-u.jp

Graduate School of Science, Nagoya University
Total No. of Pointings(N/A)

Abstract:
The ASTRO-F All-Sky Survey is an unbiased infrared survey of the whole sky, following the
IRAS All-Sky Survey made in 1983. Compared to the IRAS Survey, the wavelength coverage
is extended to longer, and the spatial resolution and the point source sensitivity are
improved by a factor of several to several tens. The survey wavebands are centered at 9, 20,
60, 90, 140, and 160 microns, respectively. ASTRO-F will allocate the survey scans primarilyin Phase I, and supplemental scans in Phase II for completeness of the sky coverage and forreliability and sensitivity. The result of them, more than 90 % of the whole sky can beobserved two or three times, more than 40 % of the sky by six times, and much deeper atnear the both ecliptic poles. The products planned are a bright point source catalog at theearliest stage, two ore more faint source catalogues at later stage, as well as maps ofextended sources. Those products are expected to be a fundamental database for the next
generation of advanced observatories, for example Herschel, and JWST, and willcomplement the SIRTF mission by virtue of its wide sky coverage. The scientific fields
covered by the All-Sky Survey spread over most part of modern astronomy /astrophysics,
such as, solar-system objects, star-forming regions, young stars, Vega-like stars, late-typestars, SNRs, interstellar matter, near-by galaxies (including Magellanic Clouds), AGNs,
star-forming galaxies, large-scale structure of the universe, and cosmology. Follow-up
studies are crucial to achieve significant scientific results in many topics.

Expected Performance of Instruments
The expected performance values concerning to the All-Sky Survey are listed in Table 1. The
detection limit values are for 5 σ in one scan, though these values will possibly be updated on the
ASTRO-F URL when new test data become available. Final values will only be fixed after the
performance verification (PV) phase on orbit. By repeating scans, the detection limit can be
improved by reducing the electrical noise and the random photon noise. The spatial resolution of 9and 20 micron bands are limited by the pixel size (not a real size, but an effective size after
summing up). The resolution of longer four bands are mainly limited by the diffraction limit whichare 1.5 to 2 times larger than the pixel size listed. The comparison of the ASTRO-F performancewith SST has been made in papers (e. g. Matsuhara et al. 2005 and Shibai 2004).

Table 1. Basic Performance of Focal Plane Instruments for All-Sky Survey
Band
S9W
L20W
N60 WIDE-S WIDE-L N160

ab

Wavelength (μm)

6-11.5

14-26

65

90

140

160

Pixel Size

9.4”

10.0”

30”

30”

50”

50”

Point Source
(mJy)

80

130

1000

200

400

800

Saturation Limit
(Jy)

36

93

90 b

30 b

200

300

Diffuse Source(MJy/sr)

24

32

7.5 a

2.5 a

2a

5

Saturation Limit(GJy/sr)

-

-

0.6 b

2.3 b

3

12

in Co-Add Mode, 3 times worse in CDS Mode.
Photometric Saturation Limit

Observation Plan
For the All-Sky Survey, the survey mode operation is used. In this mode, the telescope directionscans along a circle perpendicular to the Sun with the period same as the revolution period of 100
minutes. The telescope direction can only be shifted by ± 1 degree from the direction perpendicular
to the Sun. Hence, the survey paths are nearly aligned to the ecliptic longitudinal lines. As the orbit
is a sun-synchronous one, the axis of the survey circle must be shifted with approximately 4.1
arc-minutes spacing in average. As the cross-scan width of the array is 8.2 arc-minutes (FIS-SW) or
wider, each position of the sky can ideally be observed more than two times with subsequent orbits(“hours confirmation”), and the whole sky can ideally be achieved in a half year of Phase I.

Figure 1. Result of Simulation of the sky coverage in case that the remaining time after allocation ofpointing observations is allocated to all-sky survey. Models 2 and 3 are nominal cases.

3. Data Products
It is required to make and publish various data products as soon as possible and as perfectly as
possible. Considering the case of ASTRO-F All-Sky Survey, we are planning to make and publish
the following data products (see also Table 1).
The first catalog will be the "ASTRO-F Flux of Known Sources" containing known astronomical
catalogues (primarily IRAS PSC and FSC) with the flux observed by ASTRO-F All-Sky Survey atthe same position of the sky. Addition of the longer FIR fluxes and cross checking among bothobservations is useful as it alone. This product is expected to be automatically made duringobservation.
The Bright source catalog is constructed as the next product by confirmation between two
independent point source detections in one scan above 5 σ. In case of ASTRO-F, this is not "hours"
confirmation, but has similar process to the "hours" confirmation of the IRAS survey. The coveragecan be the whole sky, and the product will be completed within one year after the end of allnecessary survey scans. The detection limit is not improved from the one-scan sensitivity.
The Faint source catalog is produced by point source extraction "after" merging all available scans.
So, the detection limit will be improved ideally by a factor of square root of Norb. If this process isapplied only to the sky for Norb ≥ 3, the detection limit is improved by almost twice. It is expected tobe needed additional 1.5 years after the Bright source catalog.
Advanced point source catalogues can be made for a limited area of the sky which has Norb ≥ 6 ormore so as to obtain much better sensitivity. The detailed plan has not been fixed yet.

Extended source images are highly required for ASTRO-F's unique sciences, and they will be madeas the second priority after point source catalogues. However, since the amount of work needed to
produce image maps depends on the detector characteristics in space (the instruments were
designed mainly for point sources not for extended sources), it is not easy at present to assess thequality of products, man power and the time needed for it. As far as areas in which the detector isstable and can be well calibrated concerned, image maps will be able to be made not so late. On thecontrary, the all-sky image will take much longer time for production.

Table 2.
Product NameASTRO-F Flux ofknown sources
Bright Source Catalog
Faint Source Catalog
Advanced Faint Source
Catalog (T. B. D.)
Deep Survey Catalog
near Poles (T. B. D.)
Extended Source
Imagelets (T.B.D.)
ASTRO-F Intensity
Maps (T.B.D.)

Data Products from All-Sky Survey
Release Date
Survey Area
FIR Detection Limit(Norb)
40,000 sq. deg.
> 200mJy (WIDE-S) During survey
Norb ≥ 2> 400mJy (WIDE-L)
40,000 sq. deg.
200mJy (WIDE-S) EOS + ≤1 yr
Norb ≥ 2
400mJy (WIDE-L)
36,000 sq. deg.
120mJy (WIDE-S) BSC + ≤1.5 yr
Norb ≥ 3
240mJy (WIDE-L)
16,000 sq. deg.
80mJy (WIDE-S)
Norb ≥ 6
160mJy (WIDE-L)
7 sq. deg.
20mJy (WIDE-S)
Norb ≥ 100
40mJy (WIDE-L)
40,000 sq. deg.
40,000 sq. deg.

References
Matsuhara, H., Shibai, H., Onaka, H., et al., "The ASTRO-F Mission: Large Area Infrared
Survey", Advances in Space Research, in press, 2005.
Pearson, C. P., Shibai, H., Matsumoto, T., et al., "ASTRO-F, super-IRAS, the All-Sky Infrared
Survey", MNRAS, 347, 1113-1129, 2004
Shibai, H., "ASTRO-F mission", Advances in Space Research, 34, 589-593, 2004.
Wada, T., Fujishiro, N., Ishihara, D., et al., "Infrared Camera (IRC) onboard ASTRO-F", in Proc.
IR Space Telescopes and Instruments, ed. J. C. Mather, SPIE-4850, 179-190, 2003.

ASTRO-F Large-Area Survey Program
Title (Abbreviation)
Title (Full)

Date: 05/08/12

LSLMC
The ASTRO-F LMC Survey
Onaka, Takashi E-mail: onaka@astron.s.u-tokyo.ac.jp

Contact Person

Department of Astronomy, Graduate School of Science,
University of Tokyo
Total No. of Pointings

866 pointings

Abstract:
This Large Area Survey (LSLMC) plans to observe about a 15-square-degree area of theLarge Magellanic cloud with the ASTRO-F/IRC using 866 pointing observations.

The area

will be observed with 5 filters (N3, S9, S11, L15, and L24) and the prism (NP) of the IRC in
the observing mode of 2-filter observation per pointing (IRC02).

These observations

together with the FIS all-sky survey observations provide a new significant database for thevarious researches of the LMC.

Particularly mid-infrared images of S11 and L15, the NIR

spectroscopy, and the FIS 4-band data are unique to the ASTRO-F, which the SST will not beable to provide.

The expected data can address a number of astrophysical problems,

ranging from birth to death of stars, including protostars, late-type stars, super nova
remnants, and interstellar medium, and give us a first insight into detailed material
circulation in a galaxy.

The 5-band + prism data can distinguish and identify the nature ofdetected objects, such as proto-stellar objects, young stellar objects, or asymptotic giant
branch (AGB) stars.

This survey is expected to detect most of Herbig Ae/Be stars and easilyfind out dusty AGB stars in the LMC.

The spectra will elucidate the physical conditions

and properties of the interstellar dust and gas in terms of the unidentified infrared bands
and the mid-infrared continuum.

We plan to provide a point source catalog within a year

after the completion of the observations, followed by a faint source catalogue, mosaic images,
and spectroscopic data.

I. Background
The Large Magellanic Cloud (LMC) offers a unique place for the study of an extragalactic object indetail owing to its proximity (~50kpc) and nearly face-on geometry.

The metallicity of the LMC is

known to be one quarter of solar. Because of these characteristics there have been a number ofsurvey projects of the LMC in various wavelengths to study and characterize its properties (HI:
Luks & Rohlfs 1992; Kim et al. 1998, Hα: Kennicutt & Hodge 1986, Soft X: Snowden & Petre 1994;
CO: Mizuno et al. 2001; NIR: Nakajima et al. 2002).

The MSX mission has provided complete MIR

data for the LMC (Egan et al. 2001), which is the deepest in the MIR at present, but whose
detection limits are 45 and 1100mJy at 8 and 21μm, respectively, and still too shallow to comparewith survey observations in other wavelengths.

Therefore a deep MIR survey of the LMC will be avery valuable database for the various astronomical researches of the LMC.
The material in a galaxy is evolved through various processes.

Stars are formed in interstellar

clouds by accreting the interstellar matter and then become young stellar objects (YSOs), such as T
Tauri stars or Herbig Ae/Be stars. Low-mass stars evolve into the Asymptotic Giant Branch (AGB),
during which they lose their envelope by mass-loss and supply dust grains and gas to theinterstellar space.

High-mass stars end their lives as supernovae and enrich the interstellar

medium with a large amount of synthesized elements.

Supernova remnants (SNRs) are created bysupernova explosion, which interact with the surrounding medium and may trigger nextstar-formation.

Interstellar grains play an important role in every aspect of these interstellar

processes, including star-formation. All of these phenomena can be studied most effectively in theinfrared, from 2–200μm, and ASTRO-F observations of the LMC will provide a first opportunity tomake a thorough study of these material circulation processes and local star-formation history of
the LMC in a galactic scale owing to its wide spectral coverage and high sensitivities together withthe sufficient spatial resolution.

Figure 1. Observation area.

The green grids indicate the field of view of the NIR/MIR-S and theyellow ones those of the MIR-L.

II. Observation Plan
We plan to carry out observations of a large area (~ 15deg2) survey of the LMC with 5 filter bands ofthe IRC – N3, S7, S11, L15, and L24 and the NIR prism (NP). We plan to make 2 filters per
pointing observations with the IRC02 mode.

The area to be observed is shown in Figure 1.

It

consists of a fan-shaped area that includes the 30Dor and molecular ridge regions, the optical bar,several supergiant shells, and supernova remnants.

The expected detection limits (5σ) are about

7μJy with N3, 60–70μJy with S7 and S11, and 120 and 310μJy with L15 and L24, respectively.
the prism mode (NP) the continuum of about 20μJy is expected to be detected with 5σ.

InHowever,the detection limits of N3 and NP are likely to be limited by confusion in crowded regions rather
than the above values.

Confusion will not be severe for the MIR bands (λ > 10μm) at all.

We will have 866 pointing observations (each field of view will overlap with the next field by 2
arcminutes) to cover the area shown in Figure 1.
the survey.

We will use about 5 orbits per day to complete

The fields of view locations of the NIR/MIR-S and the MIR-L are different, but will

overlap with each other by making observations of contiguous regions as shown in Figure 1.
Additional 20 pointing observations with the IRC04 mode (spectroscopy in the MIR) are alsoplanned to complement the present survey as part of the interstellar medium mission program(ISMGN).

III. Scientific Objectives
The ASTRO-F LSLMC will study astrophysical processes in a galaxy from the birth to death of astar.

The IRAS survey has detected protostars in the LMC only brighter than 105Lo.

The FISsurvey will drastically improve the detection limit down to (2–5) ×103Lo owing to its smaller beam
size and higher sensitivity, providing an unbiased sample of protostars for M > 10Mo in an
extragalactic object for the first time.

The IRC survey can detect Elias 29 at the distance of the

LMC (L~36Lo; Boogert et al. 2002) and will detect the brightest end of low-mass protostars in the
NIR to MIR.

The wide spectral coverage (3–26μm) with a sufficient number of filters enable us toeasily identify the nature of the detected objects.

Particularly the spectroscopy in the NIR (NPmode) will provide an unprecedented database for the study of point sources in the LMC.
The present survey can detect most of Herbig Ae/Be stars in the LMC and distinguish them fromother objects, such as regular Be stars.

It can also detect dusty AGB stars that have undergone

strong mass-loss (Tanabe et al. 2004).

Mid-IR data of the present observation will facilitate theclassification of M-type or C-type stars and allow us to estimate the mass-loss rate from the silicate
band emission quantitatively.
There are more than 40 SNRs known in the LMC and only 10 of them have been detected by IRAS.
The present observation will observe most of them and will study the spectral energy distribution(SED) and the interaction with the surrounding medium. The observation area includes several
supergiant shells as well.

The SED of the emission from interstellar matter with different

physical conditions (from vicinity of molecular clouds to supergiant shells) will be obtained and theevolution of interstellar matter can be investigated. The continuous coverage from 3 to 26μm andthe FIS 4 bands in the FIR will provide the NIR to FIR SED over a galactic scale for the first time,from which the properties of the unidentified infrared (UIR) bands and the MIR excess emission canbe studied with respect to the FIR emission (Onaka 2000).

IV. Data Products
We plan to produce the data products as summarized in Table 1.

We will process the imaging data

right after the observations through a standard pipeline and make it available for further study.
The first point source catalog (PSC) will be created by a standard pipeline and planned to bereleased to internal use about within one year after the completion of the observations.

A revisedversion of the PSC (Faint source catalog: FSC), which improves the detection limit of the firstcatalog, is planned to be prepared within a year after the first PSC. A mosaic image of the wholeobservation area is also planned to be made available.
years after the observations.

We hope to make it available about 4 to 5

We expect that the FSC will contain as many as 5×105 sources.

Preparation of the extended source catalog is under discussion.
Table 1. Data products plan
Product

Description

Target data of release*

Image plate

Image of one field of view

Right after observation

First Point Source Catalog

Processed through Pipeline

2008

Faint Source Catalog

Lower detection limit

2009

Mosaic Image

Mosaic images on web

2010

Extended Source Catalog

Small extended sources

TBD* The proposed schedule assumes early 2006 launch.
References
Boogert, A. C. A., et al. 2002, ApJ, 570, 708
Egan, M. P., Van Dyk, S. D., & Price, S. D. 2001, AJ, 122, 1844
Kennicutt, R. C., Jr. & Hodge, P. W. 1986, 306, 130
Kim, S., et al. 1998, ApJ, 503, 674
Luks, Th. & Rohlfs, K. 1992, A&A, 263, 41
Mizuno, N., et al. 2001, PASJ, 53, 971
Nakajima, Y., et al. 2002, Proc. SPIE 4836, 29
Onaka, T. 2000, Adv. Sp. Res. 25, 2167
Sauvage, M., Vigroux, L., & Thuan, T. X. 1990, A&A, 237, 296
Snowden, S. L. & Petre, R. 1994, ApJ, 436, L123
Tanabe, T., Kicinskas, A., Nakada, Y., Onaka, T., & Sauvage, M. 2004, ApJS, 155, 401

ASTRO-F Large-Scale Survey Program
Title (Abbreviation)
Title (Full)Contact Person

Date: 05/08/12

LSNEP
The ASTRO-F NEP Survey
Hideo Matsuhara

E-mail: maruma@ir.isas.jaxa.jp

ISAS/JAXA
Total No. of Pointings

954 pointings

Abstract:
We will perform coordinated pointing surveys toward the North Ecliptic Pole (NEP) as alarge-area survey program with ASTRO-F. The NEP survey is an ASTRO-F legacy especiallyfor extragalactic astronomy and cosmology: unveiling the dusty star-formation history of theuniverse out to z=2.5, mass assembly and large scale structure evolution of the universe out
to z=4, and the nature of the cosmic infrared background (CIRB). The NEP survey also
provides us with unique information on AGN-ULIRG connection, evolution of dwarf
galaxies, and Galactic stars.
Two kinds of surveys, ``NEP-Deep" and ``NEP-Wide" are so far planned. ``NEP-Deep" will
cover 0.5 square degree circular area with 28 pointing per FOV, while ``NEP-Wide" covers
6.2 square degrees circular area with 2 pointing observations per FOV. We aim to perform
both surveys with uniform depth for all 9 imaging bands of the infrared camera covering
2-24μm wavelengths. In total 954 pointing observations are requested (483 in phase-1).
Ground-based optical, near infrared, and radio-wave pre-surveys of the area of the NEP
survey have been obtained and analyzed, the images as well as the source catalogues will besoon open to the ASTRO-F team. Also submillimeter (with BLAST), UV (with GALEX),
X-ray (with XMM) surveys are under consideration.

Figure 1. Survey Area. Red circle : "NEP-Deep", green circle: “NEP-Wide”. Also shown are theoptical deep survey field with Subaru/Suprime-cam (brown rectangle) as well as the location of
ROSAT X-ray clusters (red diamonds, Gioia et al. 2003), other ROSAT sources (galaxies, AGN,
planetary nebulae: blue crosses) and high-z radio sources (circles, Brinkman 1999).

NIR/MIR-S

MIR-L(arcmin)(arcmin)(arc
miFigure 2. “NEP-Wide” mapping strategy when the survey is done only in Phase-1. IRC has two
FOVs: NIR/MIR-S and MIR-L, separated by 20 arcmin. Thus, if NIR/MIR-S uniformly covers
the circular area (bottom, left), MIR-L coverage is no longer uniform (bottom, right). (preparedby S. Oyabu)[Details of the NEP Survey Plan]
1) 0.5deg2 "NEP-deep" (504 pointing in total) with
Band

N2

N3

N4

S7

S9W

S11

L15

L18W

L24

λ [μm]

2.43

3.16

4.14

7.19

8.74

10.39

15.56

17.81

23.04

Flux Limit [5σ, μJy]

2.8

1.2

2.3

10.

9.2

12.

22.

31.

57.

Confusion limit *

<1

<1

<1

1

3

7.9

50

134

257

(*)

confusion limit [40beams/source] by galaxies, based on Pearson 2005)

by using 28 pointing observations {8 pointing with AOT-00-a (N2, S9W, L20W)
10 pointing with AOT-00-b (N3,S7, L15)

10 pointing with AOT-00-c (N4, S11,L24)} per FOV, andA half of pointing observations(252) in "NEP-Deep" will be executed inPhase-1, and the rest will be done in Phase-2.
2) 6.2deg2 "NEP-Wide" (450 pointing in total)
Band

N2

N3

N4

S7

S9W

S11

L15

L18W

L24

λ [μm]

2.43

3.16

4.14

7.19

8.74

10.39

15.56

17.81

23.04

Flux Limit [5σ, μJy]

12

5.5

11.

49.

39.

56.

100.

130.

270.

Confusion limit *

<1

<1

<1

1

3

7.9

50

134

257

by using 2 pointing per FOV with AOT-03 (three filter mode).
About a half of pointing observations (231) in "NEP-Wide" will be executed in Phase-1.
(NOTE: observation strategy has been changed. See Appendix)
Total number of pointing is 504(deep) + 450(wide) = 954 .

Appendix. Detailed Study of “NEP-Wide” mapping Strategy
Originally “NEP-Wide” was planned to be executed only in Phase-1 : however, during the recent
detailed consideration of the mapping strategy, the survey area is found to be seriously non-uniform(see Figure 2). If we insist to keep the map uniform, we have to do with a half-circular area (seeFigure 3), which no longer overlap well with the ground pre-survey areas (CFHT/Megacam, 2deg2 &WSRT(radio), 1deg2).

Therefore, we decided to separate the “NEP-Wide” observations in bothPhase-1 and Phase-2(1st 6 months) like “NEP-Deep”. The resulted performance of the areal
coverage is shown in Figure 4.
This means the increase (219 pointings) of the NEP survey executed in Phase-2, however, if a partof MP targets near NEP (approximately 230, from SPICY and CLEVL) will be observed in Phase-1,
this NEVER affect the overall scheduling of the Mission Program and the Open Time Program, andthe all-sky survey products.

:

Figure 3. Alternative survey area of “NEP-Wide”, when the survey is done only inPhase-1. Mapping strategy is the same as that of the LMC survey, and resulted
coverage is shown by the half-circular area. Orientation of this half circular area
depends on the starting date of Phase-1.

Figure 4. MIR-L survey area of “NEP-Wide”, when the observations are made in bothPhase-1 and Phase-2 (1st 6 months) with periodic allocation of pointing opportunities,
1.25 pointing per day. (prepared by S. Oyabu)

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)AFSAS
ASTRO-F Studies on Star formation and Star forming regions

Ueno, Munetaka

PI

Co-Is

Date: 05/08/08

E-mail:ueno@provence.c.u-tokyo.ac.jp

University of Tokyo
Kitamura, Yoshimi, ISAS/JAXA
Kataza, Hirokazu, ISAS/JAXA(Continued on the next page)

Related SAC Members

M.Tamura, T.Hasegawa

Science Working GroupSF (Star Forming Regions)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

× LMC survey ×

800 pointings (A=400, B=400, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:

The mission program is based on the three pillars (projects). The first project, survey of Chamaeleon region, is really uniqueand an unrivaled project. ASTRO-F slow scanning mode gains her sensitivities reaching detection level of the photosphere ofstars, and also remains wide coverage enough to find out the orphan stars. Actual time scale in the proto-planetary disk will be
determined by the quantitative samples of this survey. A full use of ASTRO-F capabilities enables us to conduct an extended
survey to cover from the diffuse interstellar matter up to main sequence stars. This project is the first survey that has enoughsensitivities to detect any stages of YSOs and sufficient coverage, giving quantitative samples of stars with proto-planetary disks
born in the same cloud complex. The second project must be the legacyof ASTRO-F, as her atlas of various star forming sites,
including a deep survey for selected regions, collaboration with other heritages of Nobeyama Radio Observatory, NANTEN and
ASTE. The formation of brown dwarfs and planetary-mass objects and their abundance, and also the cut-off in the initial massfunction, are major topics in tis project. The third pillar is the astro-mineralogy. ASTRO-F’s unique capabilities in 3 micron,
20 micron and FTS spectroscopies realize detailed analyzations of interstellar dust particle with icy mantle and silicate dust in
the circumstellar disk. To know the composition of icy material is essentially important to understand the chemical processes
in the proto-planetary disk.
The whole sky survey of ASTRO-F is also very important part of the mission program, since it realizes a significant unbiased
census of starforming cores in a large number of molecular clouds. The sensitivity of the ASTRO-F survey of the whole Galactic
Plane, coupled with the small beam will detect pre-stellar cores to lower luminosity than previously detected. The 160 micron
channel will detect cooler sources than have been found in the IRAS data. The ASTRO-F survey will be the first all-Galaxy
measurement of the SED’s of sources in star formation regions, allowing estimation of density and temperature gradients ofa very large sample of young cores. ASTRO-F will have sufficient resolution to resolve the prestellar and protostellar clumps
within individual molecular clouds to measure the radial density profiles in the extended envelopes of the protostars. The data
will allow the measurement of temperature and density gradients, and the grain properties of material in the clouds. Viewed
from a Galaxy-wide perspective, it should help to tell us how molecular clouds fragment into cores, at what stage IMF of thestar forming region frozen in, how the disks dissipate their gas and dust, and eventually how planetary systems form in thedisks.
We are propose to use the all-sky survey data, and to conduct slow-scanning observations and spectroscopic observations ofprotoplanetary disks around low-and intermediate-mass pre-main-sequence stars with the ASTRO-F. Our main goal is to reveal
the evolution of the disks in the possible planet building stage of ∼10 Myr. The target list of this study consists of T Tauriand Herbig Ae/Be stars mainly located in the Chamaeleon and Taurus regions (d = 140 pc): the total number of the sources is∼1500. This study will be done in the following two steps: First, we will perform a photometric survey of the disks around thepre-main-sequence stars with the FIS and the IRC in the survey mode. Second, we will make spectroscopic observations over 2
200 mm of the disks detected at the 1-st step toward the weak-line T Tauri and Herbig Ae/Be stars with ages of ∼10 Myr: thenumber of the pointings is roughly estimated to be 1000. Since the Astro-F survey can detect the circumstellar disks with very
high sensitivity in gas mass of MEarth, we will be able to unveil the evolution of disk dust mass with good statistics during the
weak-line T Tauri stage of ∼10 Myr. This survey is one of the most sensitive surveys of weak-line T Tauri stars over the wholesky. Furthermore, from the successive spectroscopic observations, we can obtain the detailed spectral energy distributions of
the disks and can discuss the evolution of disk internal structures (i.e., the disk clearing in the innermost regions) relevant toplanet building at ∼10 Myr. Our large sample over several star-forming regions also makes it possible to understand how thedisk evolution depends on stellar masses and formation sites.

UENO AFSAS

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

AFSAS

PI

Date: 05/08/08

Ueno, Munetaka

Co-Is:(Continued from the previous page)
Kawamura, Akiko, Nagoya University
Okamoto, Yoshiko, Ibaragi University
Honda, Mitsuhiko, ISAS/JAXA
Sunada, Kazuyoshi, Nobeyama Radio Observatory, NAOJ
Nakazato, Takeshi, Nobeyama Radio Observatory, NAOJ
Miyazaki, Atsushi, Nobeyama Radio Observatory, NAOJ
Aikawa, Yuri, Kobe University
Ohnishi, Toshikazu, Nagoya University
Dobashi, Kazuhito, Tokyo Gakugei University
Kandori, Ryo, National Astronomical Observatory
Naoi, Takahiro, ISAS/JAXA
Fukagawa, Misato, Nagoya Tokyo
Momose, Munetake, Ibaragi University
Sugimoto, Kanako, Nagoya University
Murakawa, Koji, ASTRON
Lee, Chang Won, Korea Astronomy Observatory
Koo, Bon-Chul, Seoul National University
Park, Yong-Sun, Seoul National University
Pak, Soojong, Korea Astronomy Observatory
Toth, L. Viktor, ELTEWhite, Glenn J., The Open University
Murakami, Hiroshi, ISAS/JAXA
Tatematsu, Kenichi, National Astronomical Observatory
Hasegawa, Tetsuo, National Astronomical Observatory
Tamura, Motohide, National Astronomical Observatory

UENO AFSAS

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

AGBGA
Mass loss and stellar evolution in the AGB phase

Nakada, Yoshikazu
E-mail: nakada@kiso.ioa.s.u-tokyo.ac.jp
University of Tokyo
Toshihiko Tanabe (U. Tokyo)
Noriyuki Matsunaga (U. Tokyo)(Continued on the next page)

Related SAC Members

Y.Nakada

Science Working GroupSTAR (Stars)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

× LMC survey°

224 pointings (A=112, B=112, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:
We propose a systematic study of mass loss from AGB stars in the Milky Way globular clusters
and the nearby dwarf galaxies. The targets are selected so that they span a wide range of age andmetallicity.
The observations will be performed using the IRC and FIS pointing modes. The IRC images will
be taken in six bands, N2, N4, S7, S11, L15, and L24. They are designed to provide informationof mass-loss rate, silicate band strength, C-/M- star distinction, and stellar luminosity. The FIS
observations are carried out only to globular clusters, in order to estimate total amount of mass
lost from the stars in the system.
We plan to to make a point source catalog for each system. The evaluation of mass-loss rates fora number of AGB stars will be performed on this catalog. We will systematically investigate theeffects of metallicity and stellar mass on the mass loss phenomena. The results will be of great
importance on the understanding of the late evolution of low- to intermediate-mass stars as wellas on the study of the galactic chemical evolution.

NAKADA AGBGA

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

AGBGA

PI

Date: 05/08/08

Nakada, Yoshikazu

Co-Is:(Continued from the previous page)
Hinako Fukushi (U. Tokyo)
Takashi Miyata (U. Tokyo)
Hiroyuki Mito (U. Tokyo)
Yoshifusa Ita (ISAS/JAXA)
Issei Yamamura (ISAS/JAXA)
Hideyuki Izumiura (NAOJ)
Nobuo Arimoto (NAOJ)
Chisato Ikuta (NAOJ)
Mikako Matsuura (U. Manchester)
Kyong Sok Jeong (SNU)

NAKADA AGBGA

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

AGNUL
Evolution of ULIRGs and AGNs

Nakagawa, Takao
E-mail: nakagawa@ir.isas.jaxa.jp
ISAS/JAXA
C. Dudley, NRL
J. Fischer, NRL(Continued on the next page)

Related SAC Members

Y.Taniguchi

Science Working Group

AGN (Active Galactic Nuclei)
Required Data Resources°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

×

100 pointings (A=50, B=50, C=−)

Abstract:
We propose to study the evolution of ULIRGs (ultra luminous infrared galaxies) and AGN (active
galactic nuclei) using the ASTRO-F observations. Our proposal consists of several observation
programs, which can be categorized into two; one is detailed study of nearby ULIRGs and AGN
as templates, and the other is an investigation of the evolution of these objects toward mid- tohigh-z on the basis of the knowledge obtained in the local universe.
For the detailed study near-by ULIRGs and AGNs, we propose to make systematic spectroscopic
observations of PAH features in ULIRGs and AGNs in near-infrared to make the quantitative
estimate of star-formation activity in these dusty systems. These observations are to make thebest use of the imaging spectroscopy over wide spectral regions, which is a unique capability of
ASTRO-F. We also study Spectral Energy Distribution of representative objects in several types
using the all sky survey data.
The other category is the study of the evolution of ULIRGs and AGNs to mid- and high-z universe.
We plan number-count studies in a hierarchical manner; the number count study based on theallsky survey is useful especially for the study of the evolution in mid-z universe, and medium deep
survey with multiple observations in the survey mode and deep surveys in the slow scan mode areuseful for the study of universe with higher z. We also propose slit-less spectroscopic observations
as the rst un-biassed 3-D survey in the infrared.
The proposed infrared observations are essential for the study of ULIRGs and dusty AGNs becausea large fraction of emitted energy in these galaxies are reemitted by dust in the thermal infrared.
The unique capability of ASTRO-F will enable us to make the rst systematic study of the evolutionof dusty universe.

NAKAGAWA AGNUL

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

AGNUL

PI

Date: 05/08/08

Nakagawa, Takao

Co-Is:(Continued from the previous page)
M. Shirahata, ISAS/JAXA
D. Ishihara, ISAS/JAXA
K. Kawara, ISAS/JAXA
H. Matsuhara, ISAS/JAXA
S. Matsuura, ISAS/JAXA
C. Pearson, ISAS/JAXA
Y. Tsuzuki, IoA, UT
S. Oyabu, ISAS/JAXA
Y. Sato, IoA/UT
K. Motohara, IoA/UT
E. Verner, CUA/NASA
F. Iwamuro, Kyoto U.
S. Pak, KASI
M. Gu, KAO
M. Kim, KAO
R. Priddey, Imperial College
K. Isaak, University of Cabvridge
H. Mouri, MRI
Y. Hamada, IOA/UTY. Taniguchi, Tohoku U.
P. Barthel, Groningen
M. Rowan-Robinson, IC
T. Takagi, Kent U
T. Tamagawa, Riken
H. Urata, Riken
T. Kawaguchi, NAOJ
A. Yonehara, UT
N. Kawakatsu, SISSA
K. Enya, ISAS/JAXA
Y. Oyama, ISAS/JAXA
H. Terashima, ISAS/JAXA
H. Ueda, ISAS/JAXA
W. Kim, ISAS/JAXA
T. Suzuki, ISAS/JAXA
T. Kii, ISAS/JAXA
K. Watanabe, ISAS/JAXA
M. Kawada, Nagoya U.
N. Murakami, Nagoya U.
M. Imanishi, NAOJ

NAKAGAWA AGNUL

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/09

CLEVL
Evolution of Clusters of Galaxies

Lee, HyungMok
E-mail: hmlee@astro.snu.ac.kr
Seoul National University
Myungshin Im, Seoul National University
Myung Gyoon Lee, Seoul National University(Continued on the next page)

Related SAC Members

N.Arimoto, S.Okamura

Science Working GroupGAL (Galaxies)
Required Data Resources°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

No

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

×

346 pointings (A=173, B=173, C=−)

Abstract:
In order to understand the formation and evolution of galaxies in cluster environment, we propose
to study clusters of galaxies over a wide range of redshifts using the wide-field capability of
ASTRO-F. Since different observational strategies are required for clusters at different redshifts,
we divide our program into three major components according to the redshifts of targets: low
redshift, intermediate redshift, and high redshift clusters of galaxies. For low redshift clusters (z <0.3) we focus on the effects of environment on star formation activity by choosing samples withdifferent merging stages: major merging, minor merging and quiescent clusters. For intermediateredshift clusters (0.4 < z < 1.3), we will study star formation activity, stellar mass function, andenvironmental effect on them by conducting deep NIR-MIR imaging of selected sample clusters ofgalaxies and their surrounding groups along the large scale structures at 0.4 < z < 1.3. The highredshift cluster study can provide strong, direct constraints on the formation epoch of clusters
galaxies. Since the sample of such high-z clusters is rather rare, we will focus on high-z objects
with signs of overdensity based on other observational data, such as high-z radio galaxies, QSOs,
and submm sources. Thus we propose to conduct NIR and MIR observations of overdense regions
at 1.5 < z < 3.2, and NIR observations at z > 4. Specifically, we intend to perform deep
observations centered on high-z radio galaxies around the NEP region. Overall, our program
will explore the properties of galaxies in large areas extending out to a significant distances fromcluster’s center(about Mpc), enabling us, for the first time, to investigate the interaction of clusters
and its surrounding environment over a large redshift range (0 < z < 5) in infrared. We will also
sample the same MIR star formation indicator over 0 < z < 3 which will enable us to obtain aconsistent IR SFR estimate.

LEE CLEVL

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

CLEVL

PI

Date: 05/08/09

Lee, HyungMok

Co-Is:(Continued from the previous page)
Hoseong Hwang, Seoul National University
Narae Hwang, Seoul National University
Sang-Hoon Oh, Seoul National University
Woongseob Jeong, Seoul National University
Hideo Matsuhara, ISAS/JAXA
Takehiko Wada, ISAS/JAXA
Takao Nakagawa, ISAS/JAXA
Chris Pearson, ISAS/JAXA
Woojung Kim, ISAS/JAXA
Naofumi Fujishiro, ISAS/JAXA
Masami Ouchi, STScI
Katsuhiko Shimasaku, Univ. of Tokyo
Sadanori Okamura, Univ. of Tokyo
Masayuki Akiyama, Subaru Telescope
Shinki Oyabu, ISAS/JAXA
Hidenori Watarai, OSA/JAXA
Tadayuki Kodama, NAOJ
Hitoshi Hanami, Iwate University
Toshinobu Takagi, Univ. Kent

LEE CLEVL

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

CNIRB
ASTRO-F Observations of Cosmic Near-Infrared Background Radiation

Matsuura, Shuji
E-mail: matsuura@ir.isas.jaxa.jp
ISAS/JAXA
Mitsunobu Kawada, Nagoya University
Toshio Matsumoto, JAXA/ISAS(Continued on the next page)

Related SAC Members

Y.Taniguchi

Science Working GroupCIRB (Cosmic Background)
Required Data Resources

× NEP survey°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Large Area Survey
Total No. of Pointings

All-sky survey

×

0 pointings (A=0, B=0, C=−)

Abstract:
We propose observations of cosmic near-infrared background radiation (CNIRB) by the wide area
survey at NEP of LS program. By previous background measurements in the near-infrared with
IRTS and COBE satellites, strong background excess that is too bright to be accounted for byintegrated light of faint galaxies was discovered. From a spectral signature of redshifted Ly-α inthe background spectrum, the excess is attributed to integrated light from the first generationstars (Pop-III) populated at z∼10. Motivation of this proposal is more accurate measurement andfurther study of the Pop-III background. Absolute sky brightness and its fluctuation at blank sky
will be measured by imaging observations free from the contamination by foreground stars andgalaxies, whose contribution was a major limiting factor for the accuracy of previous backgroundmeasurements with large beam sizes. The angular power spectra of the background fluctuation
will be measured in a wide range of angular scales from arcsec to degree. Based on the auto- andcross-correlation analysis for the multi-wavelength fluctuation data, the evolution and structureformation of Pop-III clusters will be investigated. In order to study further into the redshift
distribution and surrounding nebula structure of Pop-III stars, spectroscopic measurements innear- and mid-infrared will also be performed by using the data taken for SPICY-MP and SolarSystem-MP.

MATSUURA CNIRB

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

CNIRB

PI

Date: 05/08/08

Matsuura, Shuji

Co-Is:(Continued from the previous page)
Hideo Matsuhara, JAXA/ISAS
Takehiko Wada, JAXA/ISAS
Masahiro Tanaka, NAOJ
Manabu Noda, Nagoya City Science Museum
Toshinobu Takagi, Kent University
James Bock, JPL/Caltech
Brian Keating, U.C. San Diego
Asantha Cooray, U.C. Irvine
Yoshiaki Taniguchi, Tohoku University

MATSUURA CNIRB

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

FBSEP
ASTRO-F Observations of Cosmic Far-Infrared Background Radiation andDistant Infrared Galaxies in Low-Cirrus Region near South Ecliptic Pole

Matsuura, Shuji
E-mail: matsuura@ir.isas.jaxa.jp
ISAS/JAXA
Mitsunobu Kawada, Nagoya University
Hiroshi Shibai, Nagoya University(Continued on the next page)

Related SAC Members

Y.Taniguchi

Science Working GroupCIRB (Cosmic Background)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

× LMC survey ×

270 pointings (A=270, B=0, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:
We propose the ASTRO-F observations of the cosmic far-infrared background radiation (CFIRB)
and its fluctuation, resolving the background into point sources as much as possible. Objectives ofthis program are to provide, 1) accurate source counts avoiding the cosmic variance and extended
source counts toward fainter flux below the confusion limit of the ASTRO-F telescope (∼10 mJy)by the background fluctuation analysis, in order to probe infrared galaxies at z>1, 2) angularpower spectrum of the background fluctuation to study clustering and large-scale structure traced
by infrared galaxies at z∼1, 3) statistically significant number of source samples for the study of
evolution and emission mechanism of infrared galaxies including ULIRG and AGN, and finally,4) mean flux level of CFIRB minimizing the contribution of foreground galaxies. In order toaccomplish these tasks, we plan deep and wide survey in the lowest column density region near
the south ecliptic pole, in which the best sensitivity in the far-infrared can be achieved. The
survey area of more than 15 square degrees will be mapped out by the FIS slow-scan observationsin the four wave bands with the sensitivity better than the confusion limit. To identify the farinfrared background sources and discriminate the population of detected galaxies, the IRC slowscan observations in mid-infrared bands will also be done in parallel to the FIS observations. The
optical observations of R<25mag in the FIS survey area have been planned and partly finished.
These efforts are still on-going, and another optical follow-up in multi-bands from the ground arebeing planned.

MATSUURA FBSEP

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

FBSEP

PI

Date: 05/08/08

Matsuura, Shuji

Co-Is:(Continued from the previous page)
Noriko Murakami, Nagoya University
Toshio Matsumoto, JAXA/ISAS
Takao Nakagawa, JAXA/ISAS
Hideo Matsuhara, JAXA/ISAS
Takehiko Wada, JAXA/ISAS
Shinichiro Makiuti, JAXA/ISAS
Chris P. Pearson, JAXA/ISAS
Woong-Seob Jeong, JAXA/ISAS
Shinki Oyabu, JAXA/ISAS
Mai Shirahata, JAXA/ISAS
Daisuke Ishihara, JAXA/ISAS
Yasuo Doi, University of Tokyo
Tsutomu T. Takeuchi, Laboratoire d’Astrophysique de Marseille
Stephan Serjeant, Kent University
Toshinobu Takagi, Kent University
Richard Savage, University of Sussex
Yoshiaki Taniguchi, Tohoku University

MATSUURA FBSEP

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)

FISS3
FIS Serendipitous Spectroscopic Survey

Kawada, Mitsunobu
Nagoya University

PI

Date: 05/08/07

E-mail:kawada@u.phys.nagoya-u.ac.jp

All ASTRO-F members
Co-Is
Related SAC Members

Y.Taniguchi

Science Working GroupCIRB (Cosmic Background)
Required Data Resources

× NEP survey°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

No

Large Area Survey
Total No. of Pointings

All-sky survey°

0 pointings (A=0, B=0, C=−)

Abstract:
We propose to operate the Fourier Transform Spectrometer (FTS) of the FIS at the pointing
observations allocated for the IRC. It is expected that the FIS and the IRC works very wellsimultaneously, although the FOVs of both instruments are separated. The IRC is operated
in the stealing mode of the attitude control system. In that case, the detection limit for eachphotometric band of the FIS achieves source confusion limit quickly, and there are no spatial
information in sub-pixel scale. Then, the spectroscopic observation by using the FTS is effectivewith the IRC observations. In this proposal, we never request the additional pointing observations.
We propose the operation of the FTS at the IRC observations proposed by other MPs. The
observation is not systematic nor complete. If the FTS is operated at the large area surveys near
the NEP, we expected to take rather systematic and complete datasets. According to the recent
FTS performance, we can take spectra with full resolution by averaging with all pixels only forregions in |b| < 15deg. If we use the low resolution mode of the FTS, we can take spectral energy
distributions with spectral resolution of 2.5cm-1 for a few Jy sources or for regions with surface
brightness of about 10 MJy/sr by averaging all pixels. This sensitivity is improved by multiple
observations or by reducing the spectral resolution. Using the dataset of this MP , we can discuss
about the interstellar medium and, hopefully, Cosmic Infrared Background Radiation.

KAWADA FISS3

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

FISS3

PI

Date: 05/08/07

Kawada, Mitsunobu

Co-Is:(n/a)

KAWADA FISS3

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

FUHYU
FUHYU - SPITZER WELL STUDIED FIELD MISSION PROGRAM

Pearson, Chris
E-mail: cpp@ir.isas.jaxa.jp
ISAS
Hideo Matsuhara - ISAS/JAXA
Toshinobu Takagi - University of Kent
(Continued on the next page)

Related SAC Members

N.Arimoto, S.Okamura, Y.Taniguchi

Science Working GroupGAL (Galaxies)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey

× NEP survey × LMC survey ×

50 pointings (A=25, B=25, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:
We propose MIR imaging of several well studied Spitzer fields. This imaging fills in the bands
lacking from the Spitzer surveys and gives an extremely high scientific return for minimal input for
ASTRO-F. We select fields already rich in multi-wavelength data from radio to X-ray wavelengths
to optimize the impact of the ASTRO-F observations. The deepest observations at 15microns
with ISO unveiled a large population of luminous Infrared galaxies at redshifts around 0.8 thatare responsible for the peak of the cosmic infrared background (CIRB) at 140microns. Thesegalaxies are strongly evolving with co-moving densities of infrared light 40 times larger at z=1
compared to the local universe. Deep counts with Spitzer at 24microns have confirmed this strong
evolution of the infrared luminosity function from redshift unity and have also detected a new
population of luminous infrared galaxies at higher redshifts previously unpredicted by model fits
to the ISO 15micron surveys. To link these populations and break the degeneracy in contemporary
evolutionary scenarios, observations at multiple mid-infrared wavelengths that fully sample thePAH emission are demanded. In particular, observations deeper than 1mJy at 15microns will be ofparticular value in deciphering the dominant population responsible for the evolutionary upturnin the 15micron source counts. Spitzer has extremely restricted imaging capability between 824microns so ASTRO-F observations of the Spitzer fields will be vital to unravel the nature of theinfrared populations in these fields thus linking the ISO-Spitzer populations.

PEARSON FUHYU

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

FUHYU

PI

Date: 05/08/08

Pearson, Chris

Co-Is:(Continued from the previous page)
Takehiko Wada - ISAS/JAXA
Toru Yamada - NAOJ
Steve Serjeant - University of Kent
Hyung Mok Lee - Seoul National University
Myungshin Im - Seoul National University
Woong-Seob Jeong - Seoul National University/ISAS
Eiichi Egami - University of Arizona
Casey Papovich - University of Arizona

PEARSON FUHYU

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/09

GALEV
Dusty Star-Formation History of the Universe

Matsuhara, Hideo
E-mail: maruma@ir.isas.jaxa.jp
ISAS, JAXA
Takehiko Wada, JAXA
Shuji Matsuura, JAXA(Continued on the next page)

Related SAC Members

N.Arimoto, S.Okamura, Y.Taniguchi

Science Working GroupGAL (Galaxies)
Required Data Resources

× NEP survey°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Large Area Survey
Total No. of Pointings

All-sky survey

×

66 pointings (A=40, B=26, C=−)

Abstract:
One of the key scientific goals to be performed with ASTRO-F deep surveys is to unveil the
dusty star formation history of the Universe. The NEP survey, however, is not sufficient toperform this science goal. When the NEP survey will be performed, more than ten thousands ofinfrared galaxies will be detected. Since the spectroscopic follow-ups for such a large sample arestill not realistic, we should rely on the so-called “photo-z” technique: estimation of the redshiftby fitting the SED template to the obtained multi-wavelength data. Therefore, it is essentially
important to establish the reliable SED templates of various star-forming galaxies with their
physical understandings. Another weakness of the NEP survey is the lack of the far-infrared datawith sufficient depth (i.e. confusion limit by the distant galaxies) to detect even z<=1 starburst
galaxies, although the far-infrared flux is the direct measure of the star-formation rate of the
dusty galaxies. Therefore, we propose the following strategy: 1. Mid-infrared SED studies of local
star-forming galaxies in Virgo cluster, generating their SED templates (this MP). 2. The slitless
spectroscopic survey in order to obtain the unbiased SED samples upto z=1 over the NEP survey
field (separate MP : SPICY). 3. Far-infrared Deep Survey of the NEP deep survey field below
the confusion limit by the galaxies with the FIS slow-scan survey (this MP). 4. The NEP survey(LSNEP). Determine the photometric redshifts of the detected sources by using the SED templates
derived, and then we will address the evolution of the star-formation rate of the Universe withsmall uncertainties.

MATSUHARA GALEV

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

GALEV

PI

Date: 05/08/09

Matsuhara, Hideo

Co-Is:(Continued from the previous page)
Takao Nakagawa, JAXA
Youichi Oyama, JAXA
Shinki Oyabu, JAXA
Chris P. Pearson, JAXA
Woojung Kim, JAXA
Naofumi Fujishiro, JAXA
Koji Imai, JAXAMai Shirahara, JAXA
Hidenori Watarai, JAXA
Tsutomu Takeuchi, Laboratoire d’Astrophysique de Marseille
Veronique Buat, Laboratoire d’Astrophysique de Marseille
Alessandro Bosselli, Laboratoire d’Astrophysique de Marseille
Hiroyuki Hirashita, Tsukuba University
Hiroshi Shibai, Nagoya University
Toshinobu Takagi, University of Kent
Stephen Serjeant, University of Kent
Hitoshi Hanami, Iwate University
Nobuo Arimoto, NAOJ

MATSUHARA GALEV

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

ISMGN
Interstellar dust and gas in various environments of our Galaxy and nearby galaxies

Kaneda, Hidehiro
E-mail: kaneda@ir.isas.jaxa.jp
ISAS/JAXA
H. Takahashi, Univ. of Tokyo
T. Onaka, Univ. of Tokyo(Continued on the next page)

Related SAC Members

Y.Nakada, T.Hasegawa

Science Working GroupISM (Inter Stellar Medium)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

× LMC survey°

492 pointings (A=250, B=242, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:
The aim of this MP is to perform systematic studies on interstellar dust and gas in various environments of our Galaxy and nearby galaxies. Considering the ASTRO-F uniqueness, we placeparticular importance on (A) detailed MIR-FIR SED studies of interstellar dust for moderately
large (5-10 arcmin) targets, and (B) FIR imaging and MIR slit-less spectroscopic studies of interstellar gas and dust for bright targets. The ISM can be found in various neutral and ionizedphases: hot plasma, warm ionized medium, classical HII regions, warm neutral medium, and cold
neutral medium. Owing to its wide and fine spectral coverage as well as good angular resolution,
ASTRO-F is best suited to study the processing, evolution, and destruction of dust components
spatially resolved in each ISM phase, and their connection with physical and chemical conditionsof gas and star-forming activity. Our Galactic objects allow detailed studies of the ISM in various
conditions of gas phases and density, while our sample of nearby galaxies provides us much more
extensive ranges in ISM environments and star formation history; the LMC/SMC serves to bridge
the gap between our Galaxy and the other external galaxies. A membership of this program
includes several members of the UK and Korean teams; imaging analyses of the galactic plane
will be carried out in collaboration with the UK team, while the SNR survey is one of the key
observations for collaborative research with the Korean team.

KANEDA ISMGN

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

ISMGN

PI

Date: 05/08/08

Kaneda, Hidehiro

Co-Is:(Continued from the previous page)
K. Kohno, Univ. of Tokyo
Y. Doi, Univ. of Tokyo
D. Ishihara, Univ. of TokyoY. Okada, Univ. of Tokyo
I. Sakon, Univ. of TokyoY. Y. Tajiri, Univ of Tokyo
D. Tokura, Univ. of Tokyo
T. Nakagawa, ISAS/JAXA
S. Makiuti, ISAS/JAXA
A. Yasuda, ISAS/JAXA
T. Suzuki, ISAS/JAXA
T. Hasegawa, NAOJ
H. Matsuo, NAOJ
H. Nagata, NAOJ
K. Nakanishi, NAOJ
M. Tanaka, NAOJ
K. Mochizuki, Sejong Univ.
B-C Koo, SNU
S. Hong, SNU
H-G Lee, SNU
J-J Lee, SNU
W-S Jeong, SNU
S. Pak, KAO
D-S Moon, Caltech
G. White, Kent Univ.
S. Serjeant, Kent Univ.
S. K. Ghosh, TIFR
T. Kitayama, Toho Univ.
H. Shibai, Nagoya Univ.
N. Ota, RIKEN

KANEDA ISMGN

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/07

MLHES
Excavating Mass Loss History in Extended Dust Shells of Evolved Stars

Yamamura, Issei
E-mail: yamamura@ir.isas.jaxa.jp
ISAS/JAXA
Hideyuki Izumiura, Okayama Astrophysical Observatory, NAOJ, NINS, JP
Toshiya Ueta, NASA Ames Research Center/SOFIA, USA(Continued on the next page)

Related SAC Members

Y.Nakada

Science Working GroupSTAR (Stars)
Required Data Resources°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

×

200 pointings (A=100, B=100, C=−)

Abstract:
Exploiting the superb sensitivity and mapping capabilities of ASTRO-F/FIS, we will perform a
far-IR imaging survey of the circumstellar envelopes of evolved stars. Our primary goal is to fully
understand the mass loss phenomena in the latest stages of stellar evolution by tracing the historyof mass loss carved in the structure of very extended, cold dust shells around those evolved objects.
We will obtain maps of 10x20 size of those extended dust shells with FIS by detecting thermal
emission arising from cool dust grains and reconstruct the history of mass loss along the latest
stages of stellar evolution. We will systematically examine the mass-loss history during the last
1E5 years with a time resolution of 1,000 years. From our set of coherent FIS data having varietyof evolutionary state and chemistry, we will examine (1) if mass loss history can be affected bysome stellar characteristics, and if so, how it happens, (2) if mass loss variation really occurs, andif so, how it occurs, (3) if mass loss is constant over the course of the mass loss history, and if not,if there is really a superwind, and (4) if the shell structure formation really begins early in the
AGB phase. We will also perform a mid-IR imaging with IRC of some selected objects to examine
physical conditions of dust in their shells, which would greatly improve our detailed modeling for
the FIS far-IR imaging survey.

YAMAMURA MLHES

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

MLHES

PI

Date: 05/08/07

Yamamura, Issei

Co-Is:(Continued from the previous page)
Osamu Hashimoto, Gunma Astronomical Observatory, JP
Mikako Matsuura, University of Manchester Institute of Science and Technology, UK
Takashi Miyata, Kiso Observatory, Institute of Astronomy, University of Tokyo, JP
Yoshikazu Nakada, Kiso Observatory, Institute of Astronomy, University of Tokyo, JP
Yoshifusa Ita, Institute of Space and Astronautical Science, JAXA, JP
Noriyuki Matsunaga, Institute of Astronomy, University of Tokyo, JP
Toshihiko Tanabe, Institute of Astronomy, University of Tokyo, JP
Hinako Fukushi, Institute of Astronomy, University of Tokyo, JP
Takashi Tsuji, Institute of Astronomy, University of Tokyo, JP

YAMAMURA MLHES

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/07

NIRLT
Near Infrared Spectroscopy of L and T Dwarfs

Yamamura, Issei
E-mail: yamamura@ir.isas.jaxa.jp
ISAS/JAXA
T. Tsuji, Institute of Astronomy, The University of Tokyo
T. Nakajima, National Astronomical Observatory
T. Tanabe Institute of Astronomy, The University of Tokyo

Related SAC Members

Y.Nakada

Science Working GroupSTAR (Stars)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey

× NEP survey × LMC survey ×

50 pointings (A=25, B=25, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:
Ground based observations of ultracool dwarfs, including L and T dwarfs are almost limited to
the NIR short-ward of 2.5 micron, with the exceptional case of Gl 229B. Although MIR (5.012.0
micron) is observed with Spitzer, there is no possibility of the NIR spectroscopy. The NIR regionis especially important for ultracool dwarfs, because this region includes CO fundamental bands
and CH4 nu3 fundamental bands. It was suggested from a very noisy spectra of Gl229B obtainedwith the ground-based observation that CO is over-produced by the non-equilibrium process as is
known in Jupiter atmosphere. So far, the modelings of the atmospheres of brown dwarfs are mostly
based on the equilibrium chemistry including the dust formation, and to clarify the nonequilibrium
chemistry is an important next step to a more realistic modelings of the atmospheres of browndwarfs. This can also be an important preparatory step for spectroscopy and modeling of extrasolar giant planets in the near future.
We propose to observe the NIR spectra of selected L and T dwarfs by ASTRO-F. ASTRO-F
provides a unique and exclusive opportunity to take high-quality NIR spectra of ultracool dwarfs.
Its data shall progress our understanding of the atmospheres of brown dwarfs significantly. Total
number of targets listed here is 30, in which 9 are priority A and other 10 are B. Observations
will be carried out in the AOT IRC04 with a selection of NG. Two to six pointings per object,depending on their brightness, are requested.

YAMAMURA NIRLT

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

NIRLT

PI

Date: 05/08/07

Yamamura, Issei

Co-Is:(n/a)

YAMAMURA NIRLT

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/08

SOSOS
Origin and Evolution of Solar System Objects

Ueno, Munetaka
E-mail: ueno@provence.c.u-tokyo.ac.jp
University of Tokyo
Ishiguro, Masateru, ISAS/JAXA
Kwon, Suk Minn, Kangwon National University(Continued on the next page)

Related SAC Members

T.Mukai

Science Working GroupSSO (Solar System Objects)
Required Data Resources

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

× LMC survey ×

354 pointings (A=176, B=178, C=−)Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Abstract:
There are large and small bodies in our solar system, and are also other objects such as comets and dust particles, but we
do not fully understand the linkage among themselves yet. To establish a concrete idea on the inter-planetary dust (IPD)
cloud complex under the planetary system must be one of the most important issue, since the mechanism of continuous
supply of interplanetary dust particle is still in the haze of the solar system.
Big problem on the zodiacal dust cloud is its origin, since the lifetime of the interplanetary dust under the Poynting-Robertson
drag is much shorter than the age of the Solar System. ASTRO-F capabilities on good sensitivities for extended sources,
better calibration accuracy, fine spatial resolutions and spectroscopy in middle infrared bands will open a new horizon for
IPD studies. IRAS dramatically changed the smooth featureless picture of the zodiacal dust cloud by revealing numerous
bands of asteroidal debris, several narrow trails of cometary dust, and a clumpy dust ring. However, problems of calibration
drifting and half degree resolution hindered us from fully identifying dynamical origins of the IPD cloud complex in generaland of the symmetry plane’s tilt. COBE/DIRBE also mapped almost entire sky with a 0.7 arc-degree size beam and with
better calibration, and confirmed the mean motion resonance (MMR) dust ring, and an isolation of the leading and trailingblobs in the MMR feature. The mission’s coverage of the solar elongation angle is limited to very narrow span from 89 to
91 arc-degree but the mission has superbly high sensitivity and fine spatial resolution. Its pointing and calibration stability
promises to make mission products trustworthy. The spectrum of the zodiacal emission also provides essential informationon the composition and size distribution of the IPD, and it is a clue for understanding the origin and evolution of the IPD
particles. We are also going to study IPD cloud complex using ASTRO-F scanning observations, because the morphology
includes inportant hints for its origin, and also to analyze its attribute using her spectroscopic capabilities, and finally tocomprehend the IPD cloud complex problem.
On the other hand small bodies in the solar system are also very important targets as well-known samples for the primordialconditions even after the evolution, since the minor bodies such as asteroids, comets, centaurs, and EKBOs are thought tobe remnants of the planetesimals, and contain a primitive record of the initial conditions of the solar system nebula about
4.6Gy ago.

UENO SOSOS

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

SOSOS

PI

Date: 05/08/08

Ueno, Munetaka

Co-Is:(Continued from the previous page)
Ootsubo, Takafumi, Nagoya University
Hasegawa, Sunao, ISAS/JAXA
Usui, Fumihiko, ISAS/JAXA
Hong, SeungSoo, Seoul National University
Pyo, JeongHyun, Seoul National University
Sekiguchi, Tomohiko, National Astronomical Observatory
Takahashi, Shigeru, Hiroshima City University
Kinoshita, Daisuke, National Central University
Kawakita, Hideyo, Kyoto Sangyo University
Honda, Mitsuhiko, ISAS/JAXA
Sarugaku Yuki, University of Tokyo
Jun-ichi, Watanabe, National Astronomical Observatory
Mueller, Thomas G., Max-Planck-Institut fuer extraterrestrische Physik
Mukai, Tadashi, Kobe University

UENO SOSOS

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/09

SPICY
Unbiased Slit-Less Spectroscopic Survey of Galaxies

WADA, Takehiko
E-mail: wada@ir.isas.jaxa.jp
ISAS/JAXA
Youichi Ohyama, ISAS/JAXA
Toshinobu Takagi, Kent Univ.
(Continued on the next page)

Related SAC Members

N.Arimoto, S.Okamura, Y.Taniguchi

Science Working GroupGAL (Galaxies)
Required Data Resources°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

×

200 pointings (A=100, B=100, C=−)

Abstract:
Using the ABSOLUTELY UNIQUE capability of ASTRO-F’s NIR/MIR slit-less spectroscopy, we
propose an unbiased slit-less spectroscopic survey of galaxies.
The purpose of this survey is as follows. 1) Construction of the SED templates of the galaxies.
With the redshift derived from PAH/silicate features and/or emission lines, 2) Investigationsof PAH features along with the redshift, especially the MIR(PAH)/FIR(SFR) relationship. 3)
Constraint on the galaxy evolution model by the luminosity function with type-classification, notby the galaxy counts. This survey will give a clear answer to the nature of excess in ISO 15um and
SST 24um source counts around 1mJy. This survey also gives, 4) Discovery of spectroscopicallypeculiar galaxies such as ELGs, high-z QSOs, Lya/Ha emitters at the re-ionization era. 5) Strong
constrains onto origin of the EBL.
The survey will use IRC prism and grisms (NP,SG1/2,LG1/2) in the slit-less spectroscopy modeand provide large number of unbiased galaxy samples with low resolution spectrum which covers
wavelengths of 2-26 [um]. Together with FIS 4 band photometric data, the survey will provide
SED template of galaxies which cover from NIR to FIR.
Ten pointed observations in AOT04 per FOV in the NEP survey (LSNEP) area (1 sq. deg.)
will cover the sources brighter than 0.7[mJy@24um] and provide more than 600 SED template ofgalaxies.

WADA SPICY

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

SPICY

PI

Date: 05/08/09

WADA, Takehiko

Co-Is:(Continued from the previous page)
Takao Nakagawa, ISAS/JAXA
Hideo Matsuhara, ISAS/JAXA
Shuji Matsuura, ISAS/JAXA
Chirs Pearson, ISAS/JAXA
Shinki Oyabu, ISAS/JAXA
Daisuke Ishihara, ISAS/JAXA
WooJung Kim, ISAS/JAXA
Naofumi Fujishiro,ISAS/JAXA
Mai Shirahata, ISAS/JAXA
Kentaroh Watanabe,ISAS/JAXA
Mitsunobu Kawasa, Nagoya-U
Noriko Murakami, Nagoya-U
Yoshiaki Taniguchi, Tohoku-U
Masatoshi Imanishi, NOAJ
Tsutomu T. Takeuchi, Laboratoire d’Astrophysique de Marseille
Itsuki Sakon, U-Tokyo

WADA SPICY

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (1/2)
Title (Abbreviation)
Title (Full)
PI

Co-Is

Date: 05/08/09

VEGAD
Debris Disks Around Main Sequence Stars and Extra-solar Zodiacal Emissions

Murakami, Hiroshi
E-mail: hmurakam@ir.isas.jaxa.jp
ISAS/JAXA
Hirao, Takanori, Nagoya University
Hirokazu Kataza, JAXA(Continued on the next page)

Related SAC Members

M.Tamura

Science Working GroupVEGA (Vega-like Stars)
Required Data Resources°

LMC survey

Any Follow-Up or Pre-Survey Observations by Other Facilities?

Yes

Large Area Survey
Total No. of Pointings

All-sky survey°

NEP survey

×

432 pointings (A=216, B=216, C=−)

Abstract:
The main purpose of this mission program is to trace the formation and dispersal processes ofthe debris disks around main sequence stars as well as to study whether the debris disks directly
connected to the zodiacal dust or not. From the IRC and FIS all-sky survey data, new Vega-likestar candidates with relatively large infrared excess can be discovered from the sample of stars
that have not been observed with previous missions. IRC is capable of detecting stars having
large excess such as betaPic out of more than 1000 stars. FIS is useful for the stars lack ofwarm dust such as Vega. The precise relative photometry is planned to detect very faint disks,
showing less than a few percent excess from the photosphere emission. IRC (MIR-S and MIR-L)in pointing mode will mainly be used for this observation. Since this kind of ”faint disk” may be
the analog of the zodiacal dust of out solar system, the investigation of the relationship to theplanet formation is an important point of view. For this reason, more than 100 stars are selectedfrom the TPF target list considering the instruments’ specifications. In addition, some nearbystars from AFGKM spectral types, stars in Coma Berenices open clusters and known Vega-likestars will be observed to widen our knowledge of the properties of the debris disks. We are alsoplanning to use FTS for the mineralogy of the bright debris disks around betaPic, alphaPsA andHR4796 if the performances of FTS will be improved on the orbits.

MURAKAMI VEGAD

(This page is opened to the ASTRO-F team members)

ASTRO-F Mission Programme Proposal (2/2)
Title

VEGAD

PI

Date: 05/08/09

Murakami, Hiroshi

Co-Is:(Continued from the previous page)
Issei Yamamura, JAXA
Takao Nakagawa, JAXA
Sunao Hasegawa, JAXA
Masateru Ishiguro, JAXA
Mitsuhiko Honda, JAXA
Akiko Kawamura, Nagoya University
Takafumi Ootsubo, Nagoya University
Misato Fukagawa, Nagoya University
Yoshiko Okamoto, Ibaraki University
Munetaka Ueno, University of Tokyo
Shigeyuki Sako, University of Tokyo
Yoko Okada, University of Tokyo
Shinichiro Tanaka, University of Tokyo
Hisato Kobayashi, University of Tokyo
Hideaki Fujiwara, University of Tokyo
Takuya Yamashita, NAOJ
Motohide Tamura, NAOJ

MURAKAMI VEGAD