⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩,, Ᏹᐂ࣭ཎᏊ᰾≀⌮◊✲㒊㛛,, Ᏹᐂ≀⌮⌮ㄽࢢ࣮ࣝࣉ ࣓ࣥࣂ࣮ᩍᤵ  ෸ᩍᤵ ㅮᖌ  ◊✲ဨ 

Ꮫ⏕

ᱵᮧ 㞞அ
᳃ ṇኵ
ྜྷᕝ ⪔ྖ
Alexander Wagner㸦ࢭࣥࢱ࣮㸧▼ᒣ ᬛ᫂㸦HPCI ᡓ␎ࣉࣟࢢ࣒ࣛ㸧㛗㇂ᕝ ㈼஧㸦HPCI ᡓ␎ࣉࣟࢢ࣒ࣛ㸧⾜᪉ ኱㍜ 㸦࢚ࢡࢧ FS㸧⃅㇂ 㝯ಇ㸦ᇶ┙㸿㸧኱Ꮫ㝔⏕ 㸯㸲ྡ Ꮫ㢮⏕  㸵ྡ ᴫせᮏᖺᗘ㸪ᙜࢢ࣮ࣝࣉࡣ㸪ᩘᩘ್ࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ࡼࡿ◊✲࡜ࡋ࡚㸪ࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟࡢࢥ࢔
Ɇ࢝ࢫࣉၥ㢟㸪࢔ࣥࢻ࣓ࣟࢲࡢᾦ࡜ࡉࡊࡵࡁࡢ◊✲㸪㖟Ἑࣁ࣮ࣟ୰ࢆ⁻࠺ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ࡬
ࡢ࢞ࢫ㝆╔࡜ࡑࡢᗈἼ㛗ᇦᨺᑕ㸪㍽ᑕὶయィ⟬࡟ࡼࡿ➨୍ୡ௦ᫍᙧᡂ㸪ཎጞ㖟Ἑᙧᡂ࡜Ᏹᐂ෌㟁
㞳㸪AGN ࡢ㍽ᑕ࡟ࡉࡽࡉࢀࡓศᏊ㞼ࡢ㐍໬㸪୍⯡┦ᑐㄽⓗ N యィ⟬࡟ࡼࡿᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ
ྜయ㐣⛬㸪㟁Ἴ㖟Ἑ Hydra A ࡢ Radio ࣮ࣔࢻࣇ࢕࣮ࢻࣂࢵࢡ㸪㉸᪂ᫍṧ㧁 1987A ࡢ㟁Ἴᨺᑕࡢࣔࢹࣝ໬㸪ࠕிࠖࢆ⏝࠸ࡓᏱᐂࢲ࣮ࢡ࣐ࢱ࣮ࢩ࣑࣮ࣗࣞࢩࣙࣥ㸪Vlasov-Poisson ᪉⛬ᘧࢆ⏝࠸ࡓ኱つᶍᵓ㐀ᙧᡂ࡟࠾ࡅࡿࢽ࣮ࣗࢺࣜࣀࡢᩘ್ࢩ࣑࣮ࣗࣞࢩࣙࣥ㸪ࢆ᥎㐍ࡋࡓࠋࡲࡓ㸪GPU ࢆ⏝࠸ࡓ㍽ᑕ㍺㏦࣭㍽ᑕὶయࢩ࣑࣮ࣗࣞࢩࣙࣥࢥ࣮ࢻࡢ㛤Ⓨࢆ⾜ࡗࡓࠋࡉࡽ࡟㸪ほほ࡜ࡢඹྠ◊✲࡜ࡋ࡚ࣁࢵࣈࣝᏱᐂᮃ㐲㙾࡟ࡼࡿ㧗ゎീ⏬ീࢆ⏝࠸ࡓ LAE ࡢᙧែ◊✲ LAE ࡢ࢞ࢫ㏿ᗘᵓ㐀ࡢ◊✲ࢆ⾜ࡗࡓࠋࡲࡓ㸪ᏱᏱᐂ࣭⏕࿨ศ㔝㛫㐃ᦠ࡜ࡋ࡚㸪ᫍ㛫✵㛫࡟࠾ࡅࡿ࢔࣑ࣀ㓟⏕ᡂ࡜ග୙ᩧ໬ࡢ
⌮ㄽⓗ◊✲㸪⣔እᝨᫍ࡟࠾ࡅࡿගྜᡂ࢔ࣥࢸࢼᶵᵓࡢ◊✲ࢆ᥎㐍ࡋࡓࠋ ◊✲ᡂᯝ࠙ࠚ ࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟࡢෆ㒊ᵓ㐀㸸ࢥ࢔Ɇ࢝ࢫࣉၥ㢟Ᏹᐂࡢᵓ㐀ᙧᡂࡢࣃࣛࢲ࢖࣒㸪ࢥ࣮ࣝࢻࢲ࣮ࢡ࣐ࢱ࣮(CDM)ࢩࢼࣜ࢜ࡣ㸪 N యࢩ࣑࣮ࣗࣞࢩࣙ
ࣥ࡟ࡼࡿ࡜ࢲ࣮ࢡ࣐ࢱ࣮(DM)ࣁ࣮ࣟ୰ᚰ㒊࡛㉁㔞ᐦᗘࡀⓎᩓࡍࡿ(࢝ࢫࣉ)ᵓ㐀ࢆணゝࡍࡿ
(Navarro, Frenk & White 1997; Fukushige & Makino 1997)ࠋ ࡋ࠿ࡋ㸪ࡑࡢほ⤖ᯝ࡟ࡼࡿ࡜㸪▸ᑠ㖟Ἑࡢᐦᗘࡣ୰ᚰ㒊࡛Ⓨᩓࡏࡎ㸪୍ᐃ࡜࡞ࡿ(ࢥ࢔)ࡇ࡜ࡀሗ࿌ࡉࢀ࡚࠸ࡿ (Swaters et al.
2003; Spekkens et al. 2005; Oh et al. 2010)ࠋࡇࡢ⌮ㄽ࡜ほࡢ୙୍⮴ࡣ“ࢥ࢔—࢝ࢫࣉၥ㢟”࡜࿧ࡤࢀ㸪CDM ࢩࢼࣜ࢜ࡢᮍゎỴၥ㢟ࡢ୍ࡘ࡛࠶ࡿࠋ௒ᅇᡃࠎࡣ㸪“㉸᪂ᫍ⇿Ⓨ࡟ࡼࡾ▸ᑠ㖟Ἑෆࡢ࢞ࢫࡀຍ⇕࣭⭾ᙇࡋ㸪ࡸࡀ࡚ᨺᑕ෭༷࣭཰⦰ࡀ㉳ࡇࡾ෌ࡧᫍᙧᡂࡀ㉳ࡇࡿ㸪࡜࠸࠺୍㐃ࡢ㐣⛬ࡢ⧞ࡾ㏉ࡋࡢ㔜ຊሙኚື࡟ࡼࡾ࢝ࢫࣉࡀࢥ࢔࡬࡜㑄⛣ࡍࡿ࠿”ࢆ N యࢩ࣑࣮ࣗࣞࢩࣙࣥࢆ⏝࠸࡚ㄪ-32-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩࡭ࡓࠋࡇࡇ࡛ࣂࣜ࢜ࣥࡢ㔜ຊሙࡣ࿘ᮇⓗ࡟᫬㛫ኚ໬ࡍࡿእሙ࡟ࡼࡗ࡚⾲⌧ࡋࡓࠋࡑࡢ⤖ᯝࣂࣜ࢜ࣥࡢ㔜ຊሙኚືࡢ᫬㛫ࢫࢣ࣮ࣝ࡟౫Ꮡࡋ࡚ DM ࣁ࣮ࣟ࡟ᙧᡂࡉࢀࡿࢥ࢔ࡢ኱ࡁࡉࡸ఩⨨ࡀ኱ࡁࡃኚ໬ࡍࡿ஦ࡀࢃ࠿ࡗࡓࠋࡲࡓ㸪DM ࣁ࣮ࣟࡢ⢏Ꮚ⩌࡜እሙ㛫࡛㉳ࡇࡿඹ㬆ⓗ࡞⌧㇟࡟ᑐࡍࡿゎᯒⓗ࡞ࣔࢹࣝࢆᵓ⠏ࡋࡓࠋࡇࡢඹ㬆ࣔࢹࣝ࡟ࡼࡗ࡚㸪ࢥ࢔༙ᚄࡀ㔜ຊሙࡢ᫬㛫ኚື࿘ᮇ࡜㛵ಀࡀ࠶ࡿࡇ࡜ࢆ✺ࡁṆࡵࡓࠋࡲࡓ㸪㖟Ἑࡢᙧᡂ᫬ᮇ࡜ࢥ࢔㒊ศࡢᐦᗘ࡜ࡢ㛵ಀࢆᑟࡁฟࡋࡓࠋ
࠙ࠚ ࢔ࣥࢻ࣓ࣟࢲࡢᾦ࡜ࡉࡊࡵࡁ
㏆ᖺ㸪ࣁࢵࣈࣝᏱᐂᮃ㐲㙾ࡸࡍࡤࡿᮃ㐲㙾࡟௦⾲ࡉࢀࡿᆅୖ኱ᆺᮃ㐲㙾ࢆ᭱኱㝈ά⏝ࡋࡓ㏆ഐࡢ῝Ᏹᐂ᥈ᰝ࡟ࡼࡾ㸪⌧ᅾࡶ⥆ࡃ㖟Ἑ㐍໬ࡢ㐣⛬ࢆᇉ㛫ぢࡿࡇ࡜ࡀ࡛ࡁࡿࡼ࠺࡟࡞ࡗ࡚ࡁࡓࠋ࢔
ࣥࢻ࣓ࣟࢲ㖟Ἑ࿘㎶࡟࠾࠸࡚ࡣ㸪࠾ࡧࡓࡔࡋ࠸ᩘࡢᬯ࠸▸ᑠ㖟ἙࡀⓎぢࡉࢀࡿ࡜࡜ࡶ࡟㸪ࡑࢀࡽ▸ᑠ㖟Ἑࡢ⾪✺࡟ࡼࡿࡶࡢ࡜ᛮࢃࢀࡿࢫࢸ࣮ࣛࢫࢺ࣮࣒ࣜࡸࢫࢸ࣮ࣛࢩ࢙ࣝ➼ࡢ⑞㊧ࡀ⥆ࠎ࡜᫂ࡽ࠿࡟ࡉࢀ࡚ࡁ࡚࠸ࡿࠋ≉࡟࢔ࣥࢻ࣓ࣟࢲࡢᾦ㸦࢔ࣥࢻ࣓ࣟࢲࢫࢺ࣮࣒ࣜ㸧࡟㛵ࡋ࡚ࡣ㸪ほ࣭⌮ㄽࡢ୧㠃࠿ࡽࡢ◊✲ࡀ㐍ᒎࡋ࡚ࡁ࡚࠾ࡾ㸪㖟Ἑ⾪✺ࡢ㝿ࡢ㌶㐨㐠ືࡸࡑࡢ᫬ᮇ㸪⾪✺ࡋࡓ㖟Ἑࡢ㉁㔞ࡸ໬Ꮫ⤌ᡂ➼࡟ࡘ࠸࡚⌮ゎࡀ㐍ࢇ࡛ࡁ࡚࠸ࡿࠋᡃࠎࡣ㸪N యィ⟬࡜ 3 ḟඖࡢὶయຊᏛィ⟬ࢆ⤌ࡳྜࢃࡏࡓࣁ࢖ࣈࣜࢵࢻࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ࡼࡾ㸪࢔ࣥࢻ࣓ࣟࢲ㖟Ἑࡢ෇┙࢞ࢫ࡜▸ᑠ㖟Ἑ࡟௜㝶ࡍࡿ࢞ࢫࡢὶయຊᏛⓗ࡞┦஫స⏝ࡢヲ⣽࡟ࡘ࠸࡚ㄪ࡭ࡓࠋ㖟Ἑ෇┙࢞ࢫ࡜▸ᑠ㖟Ἑ࢞ࢫࡢ┦஫స⏝࡟ࡼࡾⓎ⏕ࡍࡿ㖟Ἑ෇┙࢞ࢫࡢὶయຊᏛⓗ࡞ᣲື࡜㸪࢔ࣥࢻ࣓ࣟࢲࡢ෇┙࢞ࢫ࡛ほࡉࢀ࡚࠸ࡿࣜࣥࢢ≧ᵓ㐀ࡢ⏕ᡂ㐣⛬࡟ࡘ࠸࡚ヲ⣽࡞ゎᯒࢆ⾜ࡗࡓࠋࡲࡓ㸪▸ᑠ㖟Ἑࡢ㌶㐨㐠ືࡢึᮇ᮲௳౫Ꮡᛶ࡟ࡘ࠸࡚኱つᶍࣃ࣓࣮ࣛࢱࢧ࣮࣋࢖ࢆ⾜࠸㸪ほࢆ෌⌧ࡍࡿ㌶㐨せ⣲ࢆồࡵࡓࠋ࠙ࠚ 㖟Ἑࣁ࣮ࣟ୰ࢆ⁻࠺ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ࡬ࡢ࢞ࢫ㝆╔࡜ࡑࡢᗈἼ㛗ᇦᨺᑕྛ㖟Ἑࡣࡑࢀࡒࢀࡢ୰ᚰ࡟ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࢆᐟࡍࠋࡲࡓ㸪㖟Ἑࡣ࿘㎶ࡢ㖟Ἑ࡜⾪✺࣭ྜయࡋ㸪྾཰ྜేࡍࡿ஦࡛ࡑࡢ㉁㔞ࢆᡂ㛗ࡉࡏ࡚ࡁࡓ࡜⪃࠼ࡽࢀࡿࠋࡇࢀࡽࡢ஦࠿ࡽ㸪㖟Ἑ⾪✺࡟ࡼࡾ⾨ᫍ㖟Ἑࡀቯࡉࢀࡓᚋࡋࡤࡽࡃࡢ㛫㸪ඖ⾨ᫍ㖟Ἑࡢ୰ᚰᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡀぶ㖟Ἑࡢࣁ࣮ࣟ
୰ࢆ⁻ࡗ࡚࠸ࡿ࡜ᮇᚅࡉࢀࡿࠋ㞄ࡢ㖟Ἑ࡛࠶ࡿ࢔ࣥࢻ࣓ࣟࢲ㖟Ἑࡣ㸪ࡇࡢ㖟Ἑ⾪✺࡟ࡼࡿ㖟Ἑ࡜ࣈࣛࢵࢡ࣮࣍ࣝࡢඹ㐍໬ࢆ⌮ㄽ࡜ほࡢ୧㠃࠿ࡽ⌮ゎࡍࡿୖ࡛㸪᭱ୖࡢᐇ㦂ሙ࡛࠶ࡿࠋヲ⣽࡞ほ࡜ᩘ್ᐇ㦂ࡢẚ㍑࡟ࡼࡾ㸪⣙ 10 ൨ᖺ᫇࡟⾨ᫍ㖟Ἑࡀ⾪✺ࡋ㸪௒⌧ᅾ㸪ඖ⾨ᫍ㖟Ἑࡢ◚∦ࡀ࢔ࣥࢻ࣓ࣟࢲ㖟Ἑ࿘㎶࡟⑞㊧࡜ࡋ࡚ṧࡗ࡚࠸ࡿ஦ࡀࢃ࠿ࡗ࡚࠸ࡿࠋࡇࡢඖ⾨ᫍ㖟Ἑࡢ୰ᚰᕧ኱ࣈࣛࢵ
ࢡ࣮࣍ࣝࡀ㸪ࣁ࣮ࣟࡢᕼⷧ࢞ࢫࢆ Bondi 㝆╔࡟ࡼࡾ྾࠸㎸ࡴ᫬࡟ᙧᡂࡉࢀࡿ㝆╔෇┙ࡢᗈἼ㛗ᇦᨺᑕࢆィ⟬ࡋࡓࠋᵝࠎ࡞᳨ฟ⿦⨨ࡢឤᗘ࡜ẚ㍑ࡋࡓ࡜ࡇࢁ㸪SKA ࡸ EVLA㸪ALMA ➼ࡢ㟁Ἴ㡿ᇦࡢ᪤Ꮡ⿦⨨᳨࡛ฟྍ⬟࡛࠶ࡿ஦ࡀࢃ࠿ࡗࡓࠋ
࠙ࠚ ㍽ᑕὶయィ⟬࡟ࡼࡿ➨୍ୡ௦ᫍᙧᡂ
ிࢥࣥࣆ࣮ࣗࢱࢆ⏝࠸࡚Ᏹᐂㄽⓗὶయィ⟬ࢆᐇ⾜ࡍࡿ஦࡛ከᩘࡢ➨୍ୡ௦ࣁ࣮ࣟࢆᙧᡂࡋ㸪ࡑࡢᚋࡑࢀࡒࢀࡢࣁ࣮ࣟ࡟ࡘ࠸࡚ 3 ḟඖ㍽ᑕὶయィ⟬ࢆᐇ⾜ࡍࡿ஦࡛㸪ึ௦ᫍࡢᙧᡂ㐣⛬ࡢゎ᫂ࢆ
-33-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩

ヨࡳࡓࠋࡑࡢ⤖ᯝ㸪୍ࡘࡢࣁ࣮ࣟෆ࡛ࡶᫍ࿘෇┙ࡢศ⿣࡟ࡼࡗ࡚」ᩘࡢึ௦ᫍࡀᙧᡂࡉࢀ࠺ࡿ஦㸪
ึ௦ᫍࡢ㉁㔞ࡣ඾ᆺⓗ࡟ 10-100 ኴ㝧㉁㔞⛬ᗘ࡜࡞ࡾ㸪ᩘ๭ྜࡣከࡃ࡞࠸ࡀኴ㝧㉁㔞࣮࢜ࢲ࣮ࡢึ
௦ᫍࡸ㸪100 ኴ㝧㉁㔞ࢆ㉸࠼ࡿ኱㉁㔞ࡢึ௦ᫍࡶᙧᡂࡉࢀࡿ஦ࢆ᫂ࡽ࠿࡟ࡋࡓࠋࡲࡓ㸪ึ௦ᫍࡢ㉁㔞㸪ศ⿣㢖ᗘࡣ㸪ẕࣁ࣮ࣟ୰ᚰ㒊ࡢ࢞ࢫࡢゅ㐠ື㔞࡜ᙉ࠸┦㛵ࡀ࠶ࡿ஦ࡶࢃ࠿ࡗࡓࠋᚓࡽࢀࡓ
ึ௦ᫍࡢ㉁㔞㛵ᩘࢆ㍍࠸᪉࡟ 0.2dex ࢩࣇࢺࡉࡏࡓሙྜ࡟ண᝿ࡉࢀࡿ࣒ࣞࢼࣥࢺࡢ࢔ࣂࣥࢲࣥࢫ
ࣃࢱ࣮ࣥࡣ㸪㖟Ἑࣁ࣮ࣟ㔠ᒓḞஈᫍࡢࡑࢀ࡜ࡼࡃ୍⮴ࡍࡿࠋࡇࢀࡣ㸪ࢩ࣑࣮ࣗࣞࢩࣙࣥ⤖ᯝࡣ㸪ᩘ್ィ⟬ศゎ⬟ࡢ୙㊊࡞࡝ࡢ⌮⏤࠿ࡽ㸪ึ௦ᫍึᮇ㉁㔞㛵ᩘୖ㝈್࡜࡞ࡗ࡚࠸ࡿ஦࡟㉳ᅉࡋ࡚࠸ࡿ࡜ண᝿ࡉࢀࡿ(Susa, Hasegawa, Tominaga submitted to ApJ)ࠋ
࠙ࠚ ཎጞ㖟Ἑᙧᡂ࡜Ᏹᐂ෌㟁㞳Ᏹᐂࡣ㉥᪉೫⛣ z=1000 ⛬ᗘ୍࡛ᗘ୰ᛶ໬ࡋ㸪ࡑࡢᚋᙧᡂࡉࢀࡓኳయ࠿ࡽࡢ㍽ᑕ࡟ࡼࡗ࡚෌ࡧ
㟁㞳ࡀ㉳ࡇࡾ㸪⌧ᅾࡢᏱᐂࡣ࡯ࡰ᏶඲㟁㞳≧ែ࡛࠶ࡿ஦ࡀ▱ࡽࢀ࡚࠸ࡿࠋࡋ࠿ࡋ㸪ࡇࡢᏱᐂ෌㟁㞳ࡀࠕ࠸ࡘࠖ
ࠕ࡝ࡢኳయ࡟ࡼࡗ࡚ࠖ
ࠕ࡝ࡢࡼ࠺࡟ࠖᘬࡁ㉳ࡇࡉࢀࡓ࠿ࡣᮍࡔ᫂ࡽ࠿࡟ࡉࢀ࡚࠸࡞࠸ࠋ
ࡑࡇ࡛㸪ᡃࠎࡣ⊂⮬࡟㛤Ⓨࡋࡓࢶ࣮ࣜᵓ㐀ࢆ⏝࠸࡚㧗㏿࡟㍽ᑕ㍺㏦ィ⟬ࢆ⾜࠼ࡿࢫ࣮࣒࢟
START (SPH with Tree-based Accelerated Radiative Transfer) (Hasegawa & Umemura 2010)ࢆᏱᐂㄽⓗ㍽ᑕὶయィ⟬࡟ᑐᛂ࡛ࡁࡿࡼ࠺࡟ᣑᙇࡋ㸪ࡇࢀࢆ⏝࠸࡚Ᏹᐂ෌㟁㞳ࢩ࣑࣮ࣗࣞࢩࣙࣥ
ࢆ⾜ࡗࡓࠋࡑࡢ⤖ᯝ㸪Ᏹᐂࡢᫍᙧᡂྐࡣ୺࡟ගຍ⇕ຠᯝ࡟ࡼࡗ࡚ⴭࡋࡃ㜼ᐖࡉࢀࡿ஦ࢆ♧ࡋࡓ(Hasegawa & Semelin 2013)ࠋࡲࡓ㸪෌㟁㞳㐣⛬࡟࡜ࡗ࡚㔜せ࡞㘽࡜࡞ࡿ㟁㞳ගᏊࡢ㖟Ἑ࠿ࡽࡢ⬺ฟ๭ྜࡣ㸪⣸እ⥺ࡢࣇ࢕࣮ࢻࣂࢵࢡ࡛㧗ᐦᗘ㡿ᇦࡀ࡞ࡽࡉࢀࡿ஦࡟ࡼࡗ࡚ୖ᪼ࡍࡿ஦ࡶศ࠿ࡗ
ࡓ(Umemura et al. 2012)ࠋࢩ࣑࣮ࣗࣞࢩࣙࣥ࠿ࡽᚓࡽࢀࡓ UV ගᗘ㛵ᩘࡣ㸪z=6-8 ࡛ほྍ⬟࡞

MUV= —18 ➼ࡼࡾ᫂ࡿ࠸㖟Ἑࡢගᗘ㛵ᩘ࡜▩┪ࡋ࡞࠸ࠋࡉࡽ࡟㸪⣸እ⥺࡟ࡼࡿ㖟Ἑᙧᡂ㐣⛬㜼ᐖࢆཷࡅࡘࡘࡶ㸪ᮍࡔぢ࠼࡞࠸ᬯ࠸㖟ἙࡀከᩘᏑᅾࡍࡿ஦ࡶ᫂ࡽ࠿࡟࡞ࡾ㸪ࡇࢀࡽపගᗘ㖟Ἑࡣᩘࡀከ࠸஦㸪㟁㞳ගᏊ⬺ฟ☜⋡ࡀ㧗࠸஦࠿ࡽ෌㟁㞳࡟࠾ࡅࡿ୺せ࡞㟁㞳ගᏊ※࡜࡞ࡗ࡚࠸ࡿ஦ࡶ
᫂ࡽ࠿࡟ࡋࡓࠋ
࠙ࠚ AGN ࡢ㍽ᑕ࡟ࡉࡽࡉࢀࡓศᏊ㞼ࡢ㐍໬άື㖟Ἑ᰾(AGN)ࡣ㸪Ᏹᐂ࡛᭱ࡶ᫂ࡿ࠸ኳయࡢ 1 ࡘ࡛࠶ࡾ㸪ࡑࡢගᗘࡣ㖟Ἑᮏయ࡟༉ᩛࡍࡿࠋ
ගࡢ኱㒊ศࡣ㸪㟁㞳⬟ຊࢆᣢࡗࡓ⣸እග㸪ཬࡧ㸪X ⥺ࡢἼ㛗ᖏ࡛ᨺᑕࡉࢀࡿࡓࡵ㸪ẕ㖟Ἑࡢ㐍໬࡟኱ࡁ࡞ᙳ㡪ࢆ୚࠼ࡓ࡜୍⯡࡟⪃࠼ࡽࢀ࡚࠸ࡿࠋࡋ࠿ࡋ㸪AGN ࡢάືᛶࡢヲ⣽ࡀ࡝ࡢࡼ࠺࡟Ỵᐃࡉࢀࡿ࠿ࡣ᫂ࡽ࠿࡛࡞࠸ࠋᮏ◊✲࡛ࡣ㸪AGN ⌧㇟ࡢᣢ⥆ᛶࡢ⌮ゎࢆ㐍ࡵࡿࡇ࡜ࢆ┠ⓗ࡜ࡋ࡚㸪࢞ࢫ౪⤥࡟㔜せ࡞ᙺ๭ࢆᯝࡓࡍ࡜ᮇᚅࡉࢀࡿගᏛⓗ࡟ཌ࠸ศᏊ㞼ࡢ 1 ḟඖཬࡧ 3 ḟඖ㍽ᑕὶయィ⟬ࢆ⾜ࡗࡓࠋࡑࡢ⤖ᯝ㸪㟁㞳ࣃ࣓࣮ࣛࢱ࡜࿧ᛂᏛⓗཌࡳ࡟ᛂࡌ࡚㸪ศᏊ㞼ࡢ㐍໬ࡣග⵨Ⓨ㥑ືᆺ(I)࡜㍽ᑕᅽ㥑ືᆺ(II)࡟኱ู࡛ࡁࡿࡇ࡜ࡀࢃ࠿ࡗࡓࠋ୚࠼ࡽࢀࡓ㟁㞳ࣃ࣓࣮ࣛࢱ࡟ᑐࡋ㸪ගᏛⓗཌࡳࡀᑠࡉ࠸ሙྜࡣ I ᆺࡢ㐍໬ࢆ♧ࡋ㸪ගᏛⓗཌࡳࡀ༑ศ࡟኱ࡁ࠸ሙྜࡣ II ᆺࡢ㐍໬ࢆ♧ࡍࠋI ᆺࡢ-34-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ሙྜ㸪⌫ᑐ⛠ⓗ࡞ග⵨Ⓨ࡟ࡼࡗ࡚㉁㔞ࢆኻ࠸࡞ࡀࡽ㸪ࡑࡢ཯స⏝࡟ࡼࡿᅽຊ࡛㸪ศᏊ㞼ࡢ୍㒊ࡀ㔜ຊᔂቯ࡟⮳ࡿࠋ୍᪉㸪II ᆺࡢሙྜ㸪㍽ᑕᅽࡀග⵨ⓎὶࢆศᏊ㞼⾲㠃࡟㛢ࡌ㎸ࡵ࡞ࡀࡽ㸪㉁㔞ࢆ࡯࡜ࢇ࡝ኻࢃࡎ࡟ศᏊ㞼ࢆᢲࡋࡘࡪࡋ㸪᭱⤊ⓗ࡟ࡣศᏊ㞼ࡢ୍㒊ࢆ㔜ຊᔂቯࡉࡏࡿࡇ࡜ࡀࢃ࠿ࡗ
ࡓࠋศᏊ㞼ࡢᑑ࿨ࡣ⿕↷ᑕ㠃࡛Ⓨ⏕ࡍࡿ⾪ᧁἼࡢ㏿ᗘ࡜ศᏊ㞼ࡢࢧ࢖ࢬ࡛Ỵᐃࡉࢀࡿࠋᡃࠎࡣ 1ḟඖ㍽ᑕὶయィ⟬࡟ࡼࡾ㸪ᗈ࠸⠊ᅖࡢ㟁㞳ࣃ࣓࣮ࣛࢱ࡜ගᏛⓗཌࡳ࡟ࡘ࠸࡚㸪ศᏊ㞼ࡢᑑ࿨ࢆᐃࡋࡓࠋࡇࡢ⤖ᯝ࡟ᇶ࡙ࡃ࡜㸪ࡶࡋ AGN ࢺ࣮ࣛࢫࡀ㠀ᖖ࡟ volume filling factor ࡢᑠࡉ࠸ࢡࣛࣥ
ࣆ࣮ᵓ㐀ࢆࡋ࡚࠸ࡿ࡜ࡍࢀࡤ㸪ࢺ࣮ࣛࢫ⾲ᒙࡢ࢞ࢫࢡࣛࣥࣉࡣࢺ࣮ࣛࢫࡢຊᏛⓗ᫬㛫࡟ẚ࡭࡚㠀ᖖ࡟▷࠸᫬㛫࡛◚ቯࡉࢀࡿࡇ࡜ࡀண᝿ࡉࢀࡿࠋ
࠙ࠚ ୍⯡┦ᑐㄽⓗ N యィ⟬࡟ࡼࡿᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝྜయ㐣⛬ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡣ㖟Ἑ୰ᚰ࡟ほࡉࢀ㸪ࣈࣛࢵࢡ࣮࣍ࣝ㉁㔞ࡣ㖟Ἑࣂࣝࢪ㉁㔞ࡢ⣙ 1/1000

࡟࡞ࡗ࡚࠸ࡿ࡜࠸࠺“ࣈࣛࢵࢡ࣮̺࣍ࣝࣂࣝࢪ㉁㔞㛵ಀ”ࡀぢฟࡉࢀ࡚࠸ࡿ㸦Kormendy &Richstone 1995; Magorrian et al. 1998; Merrifield et al. 2000; Merritt & Ferrarese 2001,
Marconi & Hunt 2003㸧ࠋࡇࢀࡣ㸪ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝᙧᡂࡀ㸪㖟Ἑࣂࣝࢪᙧᡂྐ࡜ᐦ᥋࡟㛵ಀࡋ㸪ࣈࣛࢵࢡ࣮࣍ࣝ㉁㔞ࢆỴࡵࡿᬑ㐢ⓗ࡞≀⌮࣓࢝ࢽࢬ࣒ࡀᏑᅾࡋࡓࡇ࡜ࢆ♧၀ࡍࡿࠋᏱᐂࡢ㝵㝵ᒙⓗኳయᙧᡂㄽ࡟ᚑ࠼ࡤ㸪኱ࡁ࡞㖟Ἑࡣᑠ㖟Ἑࡢ㞟ྜయ࡜ࡋ࡚⏕ࡲࢀࡿࡇ࡜࡟࡞ࡾ㸪኱ࡁ࡞㖟Ἑ࡟ࡣከᩘࡢᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡀᏑᅾࡍࡿࡇ࡜࡟࡞ࡿࠋࡇࢀࡣ㸪㖟Ἑࡢ୰ᚰ࡟ࣈࣛࢵࢡ࣮̺࣍ࣝࣂࣝ
ࢪ㉁㔞㛵ಀࢆ‶ࡓࡍᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡀ୍ࡘ࠶ࡿ࡜࠸࠺ほ஦ᐇࢆㄝ࡛᫂ࡁ࡞࠸ࠋྍ⬟ᛶࡢ୍ࡘࡣ㸪㖟Ἑࡀྜయࡋࡓ㝿࡟㸪ࣈࣛࢵࢡ࣮࣍ࣝࡶ඲࡚ྜయࡋ࡚㸪㖟Ἑ୰ᚰ࡟ⴠࡕࡿ࡜࠸࠺ࡶࡢ࡛࠶
ࡿࠋࡋ࠿ࡋ㸪ࡇࢀࡲ࡛ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡢྜయࡣᴟࡵ࡚㞴ࡋ࠸࡜ࡉࢀ࡚ࡁࡓࠋᡃࠎࡣ㸪ࣈࣛࢵࢡ࣮࣍ࣝࢆᣢࡘ㖟Ἑࡀྜయࡋࡓᚋ㸪ࣈࣛࢵࢡ࣮࣍ࣝྜయࡀ㉳ࡇࡿ࠿࡜࠸࠺ၥ㢟ࢆ㸪୍⯡┦ᑐㄽຠᯝࢆධࢀࡓ㧗
㧗⢭ᗘ N యィ⟬࡟ࡼࡾㄪ࡭ࡓࠋ㖟Ἑࣂࣝࢪࡢ୰࡟ 10 ಶࡢᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࢆ⨨࠸࡚ィ⟬ࡋࡓ⤖ᯝ㸪㖟Ἑ୰ࡢᫍᐦᗘࡀ㧗࠸ሙྜ࡟ࡣ㸪ᫍ࡟ࡼࡿຊᏛⓗᦶ᧿ࡀ᭷ຠ࡟ാࡁ㸪ࣈࣛࢵࢡ࣮࣍ࣝࡣ㖟Ἑ୰ᚰ࡟ⴠࡕࡿࡇ࡜࡛ከ㔜ᩓ஘ࢆ⧞ࡾ㏉ࡋ㸪㐃ࣈࣛࢵࢡ࣮࣍ࣝࡀ⏕ࡲࢀ㸪㐃ࣈࣛࢵࢡ࣮࣍ࣝࡣ௚ࡢࣈࣛࢵࢡ࣮࣍ࣝ࡜ࡢᩓ஘ࡢ⤖ᯝ㸪㔜ຊἼࢆᨺฟࡋ࡚ྜయࡍࡿࡇ࡜ࡀศ࠿ࡗࡓࠋࡑࡋ
࡚㸪㉥᪉೫⛣ z=7 ࡢࣛ࢖࣐ࣥ࢔ࣝࣇ࢓࣭࢚࣑ࢵࢱ࣮࡛㸪ࣈࣛࢵࢡ࣮࣍ࣝྜయ㐣⛬ࡀ㉳ࡇࡗ࡚࠸ࡿ
ྍ⬟ᛶࢆ♧ࡋࡓ㸦Tanikawa & Umemura 2014㸧ࠋ

-35-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩࠙ࠚ 7KH5DGLR0RGH)HHGEDFNLQ+\GUD$

Together with collaborators at the Australian National University (Mohammad Ali Nawaz,
Geoffrey Bicknell) and the University of Waterloo (Brian McNamara) we have begun adetailed study of the famous cool-core radio galaxy Hydra A to understand the heating andmixing processes involved in radio-mode feedback on cluster scales. From existing data, wehave made accurate measurements of the hot ICM structure and the jet power usingsynchrotron minimum energy calculations. We then created realistic 2.5D relativistichydrodynamic models with the PLUTO code for the inner 30 kpc of the radio source, focusing
on the correct reproduction of conical reconfinement shocks and Mach disks. This procedureyields very accurate estimates of jet parameters, especially the jet radius, velocity, pressure,constitution, and amount of entrainment. We have also embarked upon creating. A paper has
been submitted, and is under revision, summarizing the results of the first stage of this work.
(Fig: hydra_a_shocks.png. Hydrodynamic model of the jet stream, with comparison toobservations of the jet radius and reconfinement shock locations.)࠙ࠚ 0RGHOLQJWKH5DGLRHPLVVLRQRI6XSHUQRYD5HPQDQW$In a project led by collaborator Toby Potter (University of Western Australia), we modeled
the time-dependent radio emission of supernova remnant 1987A from days 820 to 10,000
since the explosion. Following a thorough examination of the ambient ISM density structure
involving a blue supergiant wind, an HII region, and equatorial clouds, a realistic3-dimensional hydrodynamic model of the supernova expansion was performed with the-36-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩

FLASH code. The synchrotron emission from accelerated cosmic-ray electrons was calculated
by incorporating a shock detection algorithm and advecting a non-thermal particle
distribution at every shock in a semi-analytic post-process calculation involving diffusive
shock acceleration and magnetic field amplification. The resulting synthetic radio data are
directly compared with observations and shown to reproduce the global asymmetric structure
and the equatorial bright ring of emission. A paper has been submitted and accepted withminor revisions pending. (Fig: vol_obs_synth.png. Left: Volume render of the equatorial
ring-like radio emission after the interaction with dense clouds. Right: Comparison between
synthetic and observed radio data.)

࠙ࠚࠕிࠖࢆ⏝࠸ࡓࢲ࣮ࢡ࣐ࢱ࣮ࢩ࣑࣮ࣗࣞࢩࣙࣥ
ᖹᡂ 25 ᖺᗘࡣ㸪୺࡜ࡋ࡚ 2 ࡘࡢ㉁ⓗ࡟␗࡞ࡿୡ⏺᭱኱つᶍࡢࢩ࣑࣮ࣗࣞࢩࣙࣥࢆ⾜ࡗࡓࠋᅗ 1ࡢᕥࣃࢿࣝࡣ⌧ᅾࡢᏱᐂࡢ኱つᶍᵓ㐀ࢆ㸪5500 ൨ࡢࢲ࣮ࢡ࣐ࢱ࣮⢏Ꮚࢆ⏝࠸࡚ࢩ࣑࣮ࣗࣞࢩࣙࣥ
ࡋࡓࡶࡢ࡛࠶ࡿࠋྑࣃࢿࣝࡣᏱᐂึᮇ࡟ᙧᡂࡍࡿࢲ࣮ࢡ࣐ࢱ࣮ᵓ㐀ࢆ 690 ൨⢏Ꮚ࡛ࢩ࣑࣮ࣗࣞࢩ
ࣙࣥࡋࡓࡶࡢ࡛࠶ࡿࠋ࠸ࡎࢀࡶ㸪ࡑࢀࡒࢀࡢࢫࢣ࣮ࣝࡢࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥࡣୡ⏺᭱኱つᶍ࡛࠶
ࡿࠋ

-37-

⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ᅗ 1: ி࡟ࡼࡿୡ⏺᭱኱つᶍࡢࢲ࣮ࢡ࣐ࢱ࣮ࢩ࣑࣮ࣗࣞࢩࣙࣥࠋᕥࣃࢿࣝࡣ㸪⌧ᅾࡢᏱᐂࡢ኱つᶍᵓ㐀ࢆ 5500 ൨⢏Ꮚࢆ⏝࠸࡚ࢩ࣑࣮ࣗࣞࢩࣙࣥࡋࡓࡶࡢ࡛࠶ࡾ㸪࠾ࡼࡑ 50 ൨ගᖺ࡟ࢃࡓࡿ✵㛫ࡢ㖟Ἑศᕸࢆ෌⌧ࡋ࡚࠸ࡿࠋⓑᯟෆࡣᣑ኱ᅗ࡛࠶ࡾ㸪ྑୗࡢࣃࢿࣝࡣ㖟Ἑᅋࢧ࢖ࢬ(⣙ 1015 ኴ㝧㉁㔞㸧ࡢࣁ࣮࡛ࣟ࠶ࡿࠋྑࣃࢿࣝࡣ㸪Ᏹᐂึᮇ࡟ᙧᡂࡍࡿࢲ࣮ࢡ࣐
ࢱ࣮ᵓ㐀ࢆ 690 ൨⢏Ꮚࢆ⏝࠸࡚ࢩ࣑࣮ࣗࣞࢩࣙࣥࡋࡓࡶࡢ࡛࠶ࡿࠋᏱᐂㄌ⏕࠿ࡽ࠾ࡼࡑ 1൨ᖺᚋࡢᏱᐂ࡛࠶ࡾ㸪ྑୗࡢࣃࢿࣝࡣ⣙ 10-3 ኴ㝧㉁㔞ࡢࣁ࣮࡛ࣟ࠶ࡿࠋ
୧⪅ࡣఝ࡚࠸ࡿࡀ㸪࠸ࡃࡘ࠿኱ࡁ࡞㐪࠸ࡀ࠶ࡿࡇ࡜ࡀࢃ࠿ࡿࠋᏱᐂึᮇ࡟ᙧᡂࡍࡿࢲ࣮ࢡ࣐ࢱ
࣮ᵓ㐀ࡣ㸪⌧ᅾ࡟ẚ࡭⁥ࡽ࠿࡞ᵓ㐀ࢆ♧ࡋ࡚࠸ࡿࡇ࡜ࡀࢃ࠿ࡿࠋࣇ࢕࣓ࣛࣥࢺᵓ㐀ࡢ୰ࡸ㸪ࣁ࣮ࣟ࿘ᅖ࡟Ꮡᅾࡍࡿᑠࡉ࠸ࣁ࣮ࣟࡢᩘࡀᑡ࡞࠸ࡇ࡜ࡶࢃ࠿ࡿࠋ௨ୗࡑࢀࡒࢀࡢࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟
ࡘ࠸࡚㏙࡭ࡿࠋ
(i) Ᏹᐂࡢ኱つᶍᵓ㐀ᙧᡂ
ᅗ 1 ࡢᕥࣃࢿࣝ࡟ᑐᛂࡍࡿࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ࡘ࠸࡚ࡢᡂᯝ࡟ࡘ࠸࡚㏙࡭ࡿࠋ5500 ൨ࢲ࣮ࢡ࣐
ࢱ࣮⢏Ꮚࡢ㔜ຊ㐍໬ࢆ㸪୍∦࠾ࡼࡑ 50 ൨ගᖺࡢ㡿ᇦ࡛⌧ᅾࡢᏱᐂࡲ࡛ࢩ࣑࣮ࣗࣞࢩࣙࣥࡋࡓࠋึ
ᮇ᮲௳ࡣ Planck ⾨ᫍ࡟ࡼࡿ㸪CMB ࡢ᭱᪂ࡢほ⤖ᯝ࡟ᇶ࡙࠸࡚࠸ࡿࠋᑠ㖟Ἑࢫࢣ࣮ࣝ࠿ࡽᏱᐂࡢ኱つᶍᵓ㐀ࡲ࡛ศゎࡉࢀ࡚࠸ࡿࠋࢩ࣑࣮ࣗࣞࢩࣙࣥࢹ࣮ࢱࡣゎᯒ୰࡛࠶ࡿࡀ㸪௨ୗ࡟㏙࡭ࡿࡇ࡜ࡀ◊✲࡛ࡁࡿࡼ࠺࡟࡞ࡿࠋ
ࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟࡣࡑࡢࢫࢣ࣮ࣝ࡟ᑐᛂࡍࡿᵝࠎ࡞ኳయࢆᐟࡍࠋ౛࠼ࡤᡃࠎࡢ㖟Ἑ⣔ࢆࡣࡌࡵ࡜ࡍࡿࡉࡲࡊࡲ࡞㖟Ἑࡣ 1011-12 ኴ㝧㉁㔞⛬ᗘࡢࣁ࣮ࣟࡢ୰࡟ྵࡲࢀ࡚࠸ࡿ࡜⪃࠼ࡽࢀ࡚࠸ࡿࠋ
ࡲࡓ㖟Ἑᅋࡣ 1014-15㸪▸ᑠ㖟Ἑࡣ 106-10㸪ึ௦ᫍࡣ 105-7 ኴ㝧㉁㔞⛬ᗘࡢࣁ࣮ࣟ࡟Ꮡᅾࡋ࡚࠸ࡿ࡜
⪃࠼ࡽࢀ࡚࠸ࡿࠋ㖟Ἑ୰ᚰ࡟ࡣ㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡀᏑᅾࡋ㸪㖟Ἑ࡟ࡼࡗ࡚ࡣ࢞ࢫࢆࡲ࡜࠸㸪άື㖟Ἑ᰾࡜ࡋ࡚᫂ࡿࡃ㍤࠸࡚࠸ࡿࠋ㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡢ㉁㔞ࡣ㸪㖟Ἑࡢࣂࣝࢪࡢ㉁㔞࡜Ⰻࡃ┦㛵ࡋ࡚࠾ࡾ㸪ࣈࣛࢵࢡ࣮࣍ࣝ࡜㖟Ἑࡢඹ㐍໬ࢆ♧၀ࡋ࡚࠸ࡿࡀ㸪ࡑࡢᙧᡂ㸪㐍໬㐣⛬ࡣㅦ࡟-38-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ໟࡲࢀ࡚࠸ࡿࠋ
ࡇࡢࢩ࣑࣮ࣗࣞࢩࣙࣥ࡜㸪‽ゎᯒⓗ㖟Ἑᙧᡂࣔࢹࣝ࡜࠸࠺⌧㇟ㄽⓗ࡞ࣔࢹࣝࢆ⤌ࡳྜࢃࡏࡿࡇ
࡜࡛㸪ࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥࡣ┤᥋㏣ࡗ࡚࠸࡞࠸㸪ࣂࣜ࢜ࣥᡂศࡢ㐍໬ࢆ㏣࠺ࡇ࡜ࡀྍ⬟࡛࠶ࡿࠋࢩ࣑࣮ࣗࣞࢩࣙࣥୖ࡛ࡣ㸪(㞳ᩓ໬ࡉࢀࡓ)ࢲ࣮ࢡ࣐ࢱ࣮⢏Ꮚࡢᩘ༓㹼ᩘ୓ࢫࢸࢵࣉࡢ㐍໬ࢆ㏣ࡗ࡚
࠸ࡿࠋྛࢩ࣑࣮ࣗࣞࢩࣙࣥ᫬้࡟࠾࠸࡚ࡣ㸪ᩘ༑㹼ᩘ༓୓⢏Ꮚ࡛ᵓᡂࡉࢀࡿࣁ࣮ࣟࡀ↓ᩘ࡟Ꮡᅾࡋ࡚࠸ࡿࠋࢩ࣑࣮ࣗࣞࢩࣙࣥࡢࢫࢼࢵࣉࢩࣙࢵࢺࢆ 50㹼100 ⛬ᗘࡢ᫬้࡛ಖᏑࡋ࡚࠾ࡁ㸪ࡲࡎࡑࢀࡒࢀࡢࢫࢼࢵࣉࢩࣙࢵࢺ࡛ࣁ࣮ࣟࢆ᳨ฟࡍࡿ (ࡇࡢࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥࡣ⌧ᅾࡢᏱᐂ࡛࠾ࡼࡑ
ᩘ൨ࡢࣁ࣮ࣟࡀ᳨ฟࡉࢀࡿ)ࠋḟ࡟᫬้㛫࡛ྠࡌࣁ࣮ࣟࢆ⤖ࡧ௜ࡅ㸪Ᏹᐂึᮇ࠿ࡽ⌧ᅾࡲ࡛ࡢಶࠎ
ࡢࣁ࣮ࣟࡢᙧᡂྐࢆᵓ⠏ࡍࡿࠋࡇࡇ࠿ࡽඛࡀ‽ゎᯒⓗ㖟Ἑᙧᡂࣔࢹࣝࡢฟ␒࡛࠶ࡿࠋࣂࣜ࢜ࣥࡣ࠾࠾ࡼࡑࣁ࣮ࣟࡢ୰࡛㐍໬ࡋ࡚࠸ࡃࡢ࡛㸪ྛ᫬้࡛ᚓࡽࢀࡓࣁ࣮ࣟࡢᙧᡂྐࢆࡶ࡜࡟㸪⌧㇟ㄽⓗ࡞ࣔࢹࣝࢆ⏝࠸࡚㸪ಶࠎࡢࣁ࣮࡛࡛ࣟࡁࡿ㖟Ἑࡸࣈࣛࢵࢡ࣮࣍ࣝࡢᛶ㉁ࢆ⌮ㄽⓗ࡟ணゝࡍࡿࡇ࡜ࡀ࡛ࡁࡿࠋ≉࡟㧗㉥᪉೫⛣࡟࠾ࡅࡿ㖟Ἑ࡟Ꮡᅾࡍࡿάື㖟Ἑ᰾ࡣ㠀ᖖ࡟⛥࡞ኳయ࡛࠶ࡿࠋࡇࢀࡲ࡛ୡ⏺࡛⾜ࢃࢀ࡚ࡁࡓࢩ࣑ࣗ
࣮ࣞࢩ࡛ࣙࣥࡣ㸪άື㖟Ἑ᰾ࢆᐟࡍ㖟Ἑࡢ㝵ᒙⓗᵓ㐀ࢆ㏣࠺ࡔࡅࡢศゎ⬟㸪ࡲࡓࡣ⛥࡞ኳయࡀᙧ
ᡂ࡛ࡁࡿࡔࡅࡢࢩ࣑࣮ࣗࣞࢩࣙࣥయ✚ࡢ࡝ࡕࡽ࠿ࡀ୙㊊ࡋ࡚࠸ࡓࠋ௒ᅇࠕிࠖࢥࣥࣆ࣮ࣗࢱࢆ⏝࠸ࡿࡇ࡜࡛㸪ࡣࡌࡵ࡚୧᪉ࡢ᮲௳ࢆ‶ࡓࡍࡇ࡜ࡀྍ⬟࡜࡞ࡗࡓࠋࡑࡋ࡚ࡍࡤࡿᮃ㐲㙾ࡢHyper-Sprime-Cam ࡟ࡼࡗ࡚௒ᚋᩘᖺ㛫࡟ࢃࡓࡗ࡚ᚓࡽࢀࡿ㸪㧗㉥᪉೫⛣ࡢ᭱᪂ࡢほ┤᥋ẚ㍑࡛ࡁࡿࡼ࠺࡞ᗈ኱࡞㡿ᇦ࡟࠿ࡅ࡚㸪㖟Ἑ࡜ࣈࣛࢵࢡ࣮࣍ࣝࡢศᕸ୧᪉ࢆண

ࢹ࣮ࢱ࡜

ࡍࡿࡇ࡜ࡀ

࡛ࡁࡿࡼ࠺࡟࡞ࡾ㸪ඹ㐍໬㐣⛬ࡢゎ᫂࡬ࡢᡭࡀ࠿ࡾ࡞࡝ࡀᚓࡽࢀࡿࡼ࠺࡟࡞ࡗࡓࠋ
ᖹᡂ 25 ᖺᗘ୰࡟ࢩ࣑࣮ࣗࣞࢩࣙࣥ㸪࠾ࡼࡧࣁ᳨࣮ࣟฟࡣ⤊஢ࡋࡓࠋᖹᡂ 26 ᖺᗘ୰࡟㸪ࣁ࣮ࣟྜయྐࢆᵓ⠏ࡋ㸪‽ゎᯒⓗ㖟Ἑᙧᡂࣔࢹࣝ࡟ࡼࡿ㖟Ἑ+ࣈࣛࢵࢡ࣮࣍ࣝࡢᶍᨃ࢝ࢱࣟࢢࢆᵓ⠏ࡍࡿணᐃ࡛࠶ࡿࠋ

(ii) ᭱ᑠࢫࢣ࣮ࣝ࠿ࡽࡣࡌࡲࡿࢲ࣮ࢡ࣐ࢱ࣮ᵓ㐀ᙧᡂ᭱ᑠࣁ࣮ࣟ(ᆅ⌫㉁㔞)ࡣ୰ᚰࡢᐦᗘᵓ㐀ࡀ㸪༙ᚄࡢ㸫1.5 ஌⛬ᗘࡢ࡭ࡁ࡟ẚ౛ࡍࡿᛴ࡞࢝ࢫࣉᵓ
㐀ࢆࡶࡘࡇ࡜ࡀ▱ࡽࢀ࡚࠸ࡿࠋ୍᪉㸪㖟Ἑࢫࢣ࣮ࣝࡸ㖟Ἑᅋࢫࢣ࣮ࣝࡢࡼ࠺࡞኱ࡁ࠸ࣁ࣮࡛ࣟࡣ㸪
㸫1.0 ஌⛬ᗘࡢ࡭ࡁ࡛࠶ࡿࠋࡇࡢ㐪࠸ࡀ㉳ᅉࡍࡿ≀⌮࣓࢝ࢽࢬ࣒ࡣࡣࡗࡁࡾ࡜ࡣࢃ࠿ࡗ࡚࠸࡞࠸ࠋ
ࡇࡢၥ㢟ࢆ᫂ࡽ࠿࡟ࡍࡿࡓࡵ࡟ࡣ㸪᭱ᑠࣁ࣮ࣟࡀྜయࡋ࡚࡛ࡁࡿࡑࢀࡼࡾ኱ࡁ࠸ࣁ࣮ࣟࡀ࡝ࡢ
ࡼ࠺࡞ᵓ㐀࡛࠶ࡿ࠿ࢆㄪ࡭ࡿࡇ࡜ࡀ㸪ᡭ᥃࠿ࡾ࡜࡞ࡾࡑ࠺࡛࠶ࡿࠋ᭱⤊ⓗ࡞┠ᶆࡣ㸪⢏Ꮚᩘ 5500
൨㸪㡿ᇦ 800pc ⛬ᗘࡢࢩ࣑࣮ࣗࣞࢩࣙࣥࢆᐇ⾜ࡋ㸪ኴ㝧㉁㔞(106 ᆅ⌫㉁㔞)⛬ᗘࡢࣁ࣮ࣟࡢᵓ㐀ࢆㄪ࡭ࡿࡇ࡜࡛࠶ࡿࠋᖹᡂ 25 ᖺᗘࡣ㸪ணഛィ⟬࡜ࡋ࡚⢏Ꮚᩘ 690 ൨㸪㡿ᇦ 200-400pc ࡢᏱᐂㄽⓗN యࢩ࣑࣮ࣗࣞࢩࣙࣥࢆᐇ⾜ࡋ(ᅗ㸯ྑ)㸪ᩘⓒᆅ⌫㉁㔞⛬ᗘࡢࣁ࣮ࣟࡲ࡛ࡢᵓ㐀ࢆㄪ࡭ࡓࠋணഛ
ィ⟬࡛ࡣ࠶ࡿࡀ㸪ࡇࡢࢫࢣ࣮ࣝࡢࣁ࣮ࣟࡢᵓ㐀ࢆศゎࡍࡿࢩ࣑࣮ࣗࣞࢩࣙࣥ࡜ࡋ࡚ࡣ㸪ୡ⏺᭱኱
-39-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ࡢࡶࡢ࡛࠶ࡿࠋ
௒ᅇࡢࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥᚓࡽࢀࡓ㸪ࡑࢀࡽࡀྜయࡋ࡚࡛ࡁࡿࣁ࣮ࣟࡣ࡭ࡁࡀ㸫1.5 ࡼࡾὸࡃ㸪50 ᆅ⌫㉁㔞⛬ᗘࡢࣁ࣮࡛ࣟࡣ㸫1.3 ⛬ᗘ࡟࡞ࡿࡇ࡜ࡀࢃ࠿ࡗࡓࠋࣁ࣮ࣟ㉁㔞ࡀ኱ࡁࡃ࡞ࡿ࡯࡝㸪ࡼࡾ࡭ࡁࡀὸࡃ࡞ࡿഴྥ࡟࠶ࡿ㸦ᅗ 2㸧ࠋࡼࡾ኱ࡁ࠸㖟Ἑࢫࢣ࣮ࣝ௨ୖࡢࣁ࣮ࣟ(1015-21 ᆅ⌫㉁㔞)࡛ࡣ㸪ࣁ࣮ࣟࡢࢫࢣ࣮ࣝ࡟ࡼࡽࡎ㸪࡭ࡁࡀ㸫1 ⛬ᗘ࡟࡞ࡿࡇ࡜ࡀⰋࡃ◊✲ࡉࢀ࡚࠾ࡾ㸪ᆅ⌫㉁㔞
ࢆྵࡴࡑࢀ௨እࡢࢫࢣ࣮࡛ࣝࡶࡑ࠺࡛࠶ࢁ࠺࡜⪃࠼ࡽࢀ࡚࠸ࡓࠋ௒ᅇࡢ⤖ᯝࡣ 100 ಸᆅ⌫㉁㔞⛬ᗘࡢࣁ࣮ࣟࡲ࡛㸪ᚑ᮶ࡢㄝࢆそࡍࡇ࡜ࢆୡ⏺࡛ࡣࡌࡵ࡚♧ࡍࡶࡢ࡛࠶ࡿ (Ishiyama, 2014, ApJ,
788, 27)ࠋ
ࡇࡢᡂᯝࡣ௒ᚋ㸪㖟Ἑ⣔ࡢ୰ࡢࢲ࣮ࢡ࣐ࢱ࣮ᑐᾘ⁛ࢩࢢࢼࣝࢆホ౯ࡋ㸪ࢲ࣮ࢡ࣐ࢱ࣮ࡢ⣲⢏Ꮚࡢ᥈ᰝ࡜ࡑࡢヲ⣽࡞ᛶ㉁ࢆゎ᫂ࡍࡿࡓࡵ࡟ᛂ⏝ࡉࢀࡿࠋᑐᾘ⁛ࢩࢢࢼࣝࡣᒁᡤⓗࢲ࣮ࢡ࣐ࢱ࣮ᐦ
ᗘࡢᵓ㐀ࡢ 2 ஌࡟ẚ౛ࡍࡿࡓࡵ㸪ࣁ࣮ࣟࡢᚤ⣽ᵓ㐀ࡣᴟࡵ࡚㔜せ࡛࠶ࡿࠋࣁ࣮ࣟ⮬యࡢᵓ㐀⮬యࡢ௚࡟㸪ࣁ࣮ࣟෆ࡟↓ᩘ࡟Ꮡᅾࡍࡿᒁᡤⓗ఩┦✵㛫ᐦᗘࡢᴟ኱㸪࠸ࢃࡺࡿࢧࣈࣁ࣮ࣟࡢᵓ㐀㸪ศᕸࢆ᫂ࡽ࠿࡟ࡍࡿᚲせࡀ࠶ࡿࠋࡑࡢࡓࡵ࡟ࡣ࡛ࡁࡿࡔࡅ኱ࡁ࠸ࣁ࣮ࣟࢆࢩ࣑࣮ࣗࣞࢩࣙࣥࡍࡿᚲ
せࡀ࠶ࡿࠋᖹᡂ 26 ᖺᗘ࡟⾜࠺ணᐃ࡛࠶ࡿ㸪⢏Ꮚᩘ 5500 ൨ࡢࢩ࣑࣮ࣗࣞࢩࣙࣥࡣ㸪ኴ㝧㉁㔞ࡢࣁ࣮ࣟࡢᵓ㐀ࢆ᫂ࡽ࠿࡟࡛ࡁࡿࡔࡅ࡛࡞ࡃ㸪ࡇ࠺࠸ࡗࡓࢧࣈࣁ࣮ࣟ࡜ࡋ࡚ࡢ᭱ᑠࢫࢣ࣮ࣝࣁ࣮ࣟࡢ
㐍໬ࢆ㏣࠺ࡇ࡜ࡀ࡛ࡁࡿ၏୍ࡢࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥ࠶ࡿࠋ

ᅗ 2 : 2 ᆅ⌫㉁㔞(ᕥ)㸪10 ᆅ⌫㉁㔞(୰ኸ)㸪50 ᆅ⌫㉁㔞(ྑ)ࡢࣁ࣮ࣟࡢᐦᗘᵓ㐀(ୖ 3 ࣃࢿࣝ)࡜㸪ᐦᗘࣉࣟࣇ࢓࢖ࣝࡢ࡭ࡁ(ୗ 3 ࣃࢿࣝ)ࠋ㉥⥺࡜㟷⥺ࡀ㸪ᆅ⌫㉁㔞ࡢࣁ࣮ࣟࡀ࡛
ࡁࡿ≀⌮ࢆṇࡋࡃ㏣ࡗࡓࢩ࣑࣮ࣗࣞࢩࣙࣥࡢ⤖ᯝ࡛࠶ࡿࠋ⥳⥺ࡣ㸪㖟Ἑࢫࢣ࣮ࣝ࡞࡝ࡼ
ࡾ኱ࡁ࠸ࣁ࣮ࣟࡢᵓ㐀ᙧᡂྐࢆᶍೌࡍࡿࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥ࠶ࡿ (reference model)ࠋ
-40-

⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩࠙ࠚVlasov-Poisson ᪉⛬ᘧࢆ⏝࠸ࡓ኱つᶍᵓ㐀ᙧᡂ࡟࠾ࡅࡿࢽ࣮ࣗࢺࣜࣀࡢᩘ್ࢩ࣑࣮ࣗࣞ
ࢩࣙࣥ⣲⢏Ꮚᐇ㦂࡟ࡼࡿࢽ࣮ࣗࢺࣜࣀ᣺ືࡢⓎぢ࡟ࡼࡗ࡚㉁㔞ࢆᣢࡘࡇ࡜ࡀ᫂ࡽ࠿࡜࡞ࡗࡓࢽ࣮ࣗࢺ
ࣜࣀࡣ㸪Ᏹᐂึᮇ࡟┦ᑐㄽⓗ࡞≧ែ࡛௚ࡢᡂศ࠿ࡽ⬺⤖ྜࡋ࡚㸪ගᏊ࡜࡯ࡰྠࡌᩘᐦᗘ࡛኱㔞࡟Ꮡᅾࡍࡿࠋࡲࡓ㸪ࢽ࣮ࣗࢺࣜࣀࡣࡑࡢ㍍࠸㉁㔞ࡢⅭ࡟⌧ᅾࡢᏱᐂ࡟࠾࠸࡚ࡣ㖟Ἑࡢ⬺ฟ㏿ᗘ࡟༉
ᩛࡍࡿ㏿ᗘศᩓࢆᣢࡕ㸪Ᏹᐂࡢ኱つᶍᵓ㐀ࡢᙧᡂ㐣⛬࡟࠾࠸࡚㸪ᐦᗘᦂࡽࡂࡢ㔜ຊⓗᡂ㛗ࢆ↓⾪✺ῶ⾶࡟ࡼࡗ࡚㜼ᐖࡍࡿാࡁࡀ࠶ࡿࠋ㏻ᖖ㸪Ᏹᐂࡢ኱つᶍᵓ㐀ᙧᡂࡢᩘ್ࢩ࣑࣮ࣗࣞࢩࣙࣥࡣ Nయࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥ⾜ࢃࢀࡿࡀ㸪N యࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥࡣ⢏Ꮚᛶ࡟ࡼࡿࢩࣙࢵࢺࣀ࢖ࢬࡢࡓ
ࡵ࡟↓⾪✺ῶ⾶ࡢࢩ࣑࣮ࣗࣞࢩࣙࣥࢆ⢭ᗘⰋࡃィ⟬ࡍࡿࡢࡣ㞴ࡋ࠸ࠋࡑࡇ࡛㸪ᡃࠎࡣ N యࢩ࣑࣮ࣗࣞࢩࣙࣥࡢ௦ࢃࡾ࡟ Vlasov-Poisson ᪉⛬ᘧࢆ┤᥋ᩘ್ࢩ࣑࣮ࣗࣞࢩࣙࣥࡍࡿᡭἲࢆ⏝࠸࡚㸪኱つᶍᵓ㐀ᙧᡂ㐣⛬࡟࠾ࡅࡿࢽ࣮ࣗࢺࣜࣀࡢࢲ࢖ࢼ࣑ࢡࢫࢆᩘ್ࢩ࣑࣮ࣗࣞࢩࣙࣥࡍࡿࡇ࡜ࢆ┠ᣦࡋ࡚࠸ࡿࠋᮏᖺᗘࡣ㸪ࢲ࣮ࢡ࣐ࢱ࣮ࢆ N యࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥࢩ࣑࣮ࣗࣞࢩࣙࣥࡋ㸪ࢽ࣮ࣗࢺࣜ
ࣀࡢ㐠ືࢆ Vlasov-Poisson ᪉⛬ᘧࡢ┤᥋ࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥゎࡃࢥ࣮ࢻࢆ㛤Ⓨࡋࡓࠋ࠙ࠚGPU ࢆ⏝࠸ࡓ㍽ᑕ㍺㏦࣭㍽ᑕὶయࢩ࣑࣮ࣗࣞࢩࣙࣥࢥ࣮ࢻࡢ㛤Ⓨ㍽ᑕ㍺㏦ࢩ࣑࣮ࣗࣞࢩࣙࣥࡸࡑࢀࢆὶయຊᏛࢩ࣑࣮ࣗࣞࢩࣙࣥ࡜࢝ࢵࣉࣝࡉࡏࡓ㍽ᑕὶయࢩ࣑
࣮ࣗࣞࢩࣙࣥࡣ㸪㍽ᑕ㍺㏦ࢩ࣑࣮ࣗࣞࢩࣙࣥࡢィ⟬ࢥࢫࢺࡀ⭾኱࡛࠶ࡿࡓࡵ㸪ࡇࢀࡲ࡛ࡢኳయᙧ
ᡂࡢᩘ್ࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥࡣ↓どࡉࢀࡿ࠿⡆౽࡞ᡭἲ࡛㏆ఝⓗ࡟ࡢࡳィ⟬ࡉࢀࡿሙྜࡀ࡯࡜ࢇ
࡝࡛࠶ࡗࡓࠋᡃࠎࡣ㸪㍽ᑕ㍺㏦ィ⟬ࢆ GPU ࡸ࣐ࣝࢳࢥ࢔࣭࣓ࢽ࣮ࢥ࢔࢔࣮࢟ࢸࢡࢳࣕ࡟ᇶ࡙ࡃ
ࣉࣟࢭࢵࢧ࡛ຠ⋡ⓗ࡟ᐇ⾜ࡍࡿ࢔ࣝࢦࣜࢬ࣒ࢆ㛤Ⓨࡋࡓࠋࡇࡢࢥ࣮ࢻࡣ㸪Ⅼ※࠿ࡽࡢ㍽ᑕ㍺㏦ࢆ
ゎࡃ ARGOT ἲ࡜෌⤖ྜᨺᑕ࡞࡝ࡢᗈࡀࡗࡓ㡿ᇦ࠿ࡽࡢ㍽ᑕ㍺㏦ࢆゎࡃ ART ἲࢆ GPU ࡸ࣐ࣝࢳࢥ࢔ࣉࣟࢭࢵࢧ࡟࠾࠸࡚ᐇ⿦ࡋࡓࡶࡢ࡛࠶ࡾ㸪MPI ࡟ࡼࡿࣀ࣮ࢻ୪ิ໬ࡶ⾜࠸㧗࠸୪ิ໬ຠ⋡ࢆ㐩ᡂࡋࡓࠋ࠙ࠚࣁࢵࣈࣝᏱᐂᮃ㐲㙾ࡢ㧗ゎീ⏬ീࢆ⏝࠸ࡓ LAE ࡢᙧែ◊✲ ࠓほ࡜ࡢඹྠ◊✲ࠔ⊂⮬࡟ᵓ⠏ࡋࡓ 426 ಶࡢ኱つᶍ z=2.2 LAE ࢧࣥࣉࣝ࡜ࣁࢵࣈࣝᏱᐂᮃ㐲㙾ࡢ㧗ゎീ⏬ീࢆ⤌ࡳྜࢃࡏ㸪LAE ࡢ⤫ィⓗᙧែ◊✲ࢆ⾜ࡗࡓ㸬≉࡟ᡃࠎࡣ LAE ࡢࠕ(1) ྜయ㖟Ἑࡢ๭ྜࠖ
ࠕ(2) Lyǂ
࡜ᫍᡂศ㐃⥆ගࡢ✵㛫ⓗࡎࢀ(Lyǂ spatial offset; ǅLyǂ)ࠖࠕ(3) ᴃ෇⋡ (~㖟Ἑࡢぢ㎸ࡳゅࡢᣦᶆ)ࠖ
࡜ࡑࢀࡽࡢ Lyǂ ➼౯ᖜ࡬ࡢ౫Ꮡᛶࢆㄪ࡭ࡓ㸬ࡇࢀࡲ࡛࡟ࡶ LAE ࡢᙧែ◊✲ࡣ࠸ࡃࡘ࠿࠶ࡗࡓ
ࡀ㸪Lyǂ ගᏊࡢฟ᫆ࡉ(~Lyǂ ➼౯ᖜ)࡜ࡢ㛵ಀ࡟╔┠ࡋ㸪⤫ィⓗ࡟ㄪᰝࡋࡓࡢࡣ௒ᅇࡀึࡵ࡚࡛࠶
ࡿ㸬ࡇࢀ࡟ࡼࡾ㸪ࡇࢀࡲ࡛ࡢᑠࡉ࡞ࢧࣥࣉࣝ(N㹼10)ࢆ⏝࠸ࡓ◊✲࡟ࡼࡗ࡚ಙࡌࡽࢀ࡚ࡁࡓࠕ㖟Ἑྜయ࡟ࡼࡗ࡚࿘㎶㖟Ἑ≀㉁ࡀ๤ࡂྲྀࡽࢀ Lyǂ ࡢ⬺ฟࢆಁ㐍ࡍࡿࠖ࡜࠸࠺ண᝿(Cooke+2010 ࡞࡝)ࡢጇᙜᛶࡸࠕLyǂ ගᏊࡣ㖟Ἑ෇┙࡜ᆶ┤ࡢ᪉ྥ(face-on)࠿ࡽ⬺ฟࡋ᫆࠸ࠖ࡜࠸࠺⌮ㄽண᝿(Zheng &Wallance 2013 ࡞࡝)ࢆ⤫ィⓗ࡟᳨ドࡍࡿࡇ࡜ࡀ࡛ࡁࡓ㸬ㄪᰝࡢ⤖ᯝ㸪Lyǂ ➼౯ᖜࡀ኱ࡁ࡞ LAE-41-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ࡣ඾ᆺⓗ࡟ (1) 㖟Ἑྜయࡢ඙ೃࡀ࡞ࡃ㸪(2) ǅLyǂ ࡀᑠࡉࡃ㸪(3) ᴃ෇⋡ࡀᑠࡉ࠸ (ࡍ࡞ࢃࡕface-on) ࡛࠶ࡿࡇ࡜ࡀศ࠿ࡗࡓ㸬ࡇࡢࡇ࡜࠿ࡽ㸪㖟Ἑྜయࡣ࢞ࢫࢆ๤ࡂྲྀࡿ௦ࢃࡾ࡟㸪୺࡜ࡋ࡚୰ᚰ㖟Ἑࢆそ࠸㞃ࡍຠᯝࡀ࠶ࡿྍ⬟ᛶࢆ♧ࡋࡓ㸬㖟Ἑྜయ࡟ຍ࠼㸪ǅLyǂ/ᴃ෇⋡ࡢ㆟ㄽ࠿ࡽ㸪LyǂගᏊࡣࠕ࿘㎶㖟Ἑ≀㉁ࡢᰕᐦᗘࡀప࠸㡿ᇦ࠿ࡽຠ⋡ⓗ࡟ᨺᑕࡉࢀࡿࠖࡇ࡜ࡀほⓗ࡟᫂ࡽ࠿࡟࡞

ࡗࡓ (Shibuya et al. 2014a)㸬
࠙ࠚLAE ࡢ࢞ࢫ㏿ᗘᵓ㐀ࡢ◊✲ ࠓほ࡜ࡢඹྠ◊✲ࠔ 㐲᪉㖟Ἑࡢ࢞ࢫࡢ㏿ᗘᵓ㐀ࡣ㸪୰ᛶỈ⣲࢞ࢫ࡟ᑐࡋ࡚ගᏛⓗ࡟ⷧ࠸ࠕᫍ㞼⥺ࠖࢆࡑࡢ㖟Ἑࡢ⣔⤫ⓗ㏿ᗘ(ᇶ‽)࡜ࡋ࡚㸪Lyǂ ㍤⥺ࡲࡓࡣ㔠ᒓ྾཰⥺࡜ࡢ㏿ᗘᕪ (ƦvLyǂ, ƦvIS)ࢆ

ࡿࡇ࡜࡛ㄪ࡭ࡽࢀ

ࡿ㸬㏆㉥እศගჾࡢᢏ⾡Ⓨᒎ࡟ࡼࡾ㸪᫂ࡿ࠸㖟Ἑ✀᪘(LBG)ࡢࡳ࡞ࡽࡎ㸪඾ᆺⓗ࡟ᬯ࠸✀᪘࡛࠶ࡿ LAE ࠿ࡽࡶᫍ㞼⥺ࡀ᳨ฟࡉࢀ㸪ࡑࢀࡽࡢ㏿ᗘᵓ㐀ࡀㄪ࡭ࡽࢀ࡚ࡁࡓ(Chonis+2013 ࡞࡝)㸬Hashimoto+2013 ࡣ ƦvLyǂ ࡜ Lyǂ ➼౯ᖜࡢ㛫࡟㏫┦㛵ࡀ࠶ࡿࡇ࡜ࢆ♧ࡋࡓࡀ㸪ƦvLyǂ ࡣ୰ᛶỈ⣲ᰕᐦᗘ NHI ࡜࢞ࢫ ࢔࢘ࢺࣇ࣮ࣟ㏿ᗘࡢ୧᪉࡟ᩄឤ࡞≀⌮㔞࡛࠶ࡿࡓࡵ㸪ࡇࡢ㛵ಀࡢ㉳※ࡀศ࠿ࡽ࡞࠸≧ἣ࡟࠶ࡗࡓ㸬ࡑࡇ࡛ᡃࠎࡣ㸪Keck ᮃ㐲㙾/LRIS ࡞࡝ࡢศගჾࢆ⏝࠸࡚ z=2.2 LAE ࡢ
ྍど㸭㏆㉥እศගほࢆ⾜ࡗࡓ㸬ࡑࡢ⤖ᯝ㸪ࡇࢀࡲ࡛ࡢ ƦvLyǂ ࡀᐃࡉࢀࡓ LAE ࢧࣥࣉࣝࢆ 2 ಸ࡟ቑࡸࡍࡇ࡜ࡀ࡛ࡁ㸪ᥦ᱌ࡉࢀ࡚࠸ࡓ ƦvLyǂ-Lyǂ ➼౯ᖜ ㏫┦㛵ࢆ㧗࠸᭷ពᛶ࡛☜ㄆࡍࡿࡇ࡜ࡀ࡛
ࡁࡓ㸬ࡉࡽ࡟㸪LRIS ࡢ㛗᫬㛫ศගほ࡟ࡼࡾ௒ࡲ࡛ࡣ᳨ฟࡀᅔ㞴࡛࠶ࡗࡓᬯ࠸⣸እ⥺㐃⥆ග㸪ཬࡧከᩘࡢ㔠ᒓ྾཰⥺ࢆ 4 ಶࡢ LAE ࠿ࡽ᳨ฟࡍࡿࡇ࡜࡟ᡂຌࡋࡓ㸬ࡑࢀࡽࡢ(࢔࢘ࢺࣇ࣮ࣟ㏿ᗘ࡟ࡢࡳᩄឤ࡞)ƦvIS ࡣ -200~300 km/s ࡛࠶ࡾ㸪LAE ࡶ LBG ࡜ྠᵝ࡟ᙉ࠸࢔࢘ࢺࣇ࣮ࣟࢆ㉳ࡇࡋ࡚࠸ࡿࡇ࡜ࡀ᫂ࡽ࠿࡟࡞ࡗࡓ㸬ࡇࡢࡇ࡜࠿ࡽ㸪ᑠࡉ࡞ ƦvLyǂ ࢆᣢࡘ LAE ࡣࠕᑠࡉ࡞࢞ࢫ ࢔࢘ࢺࣇ࣮ࣟ㏿ᗘࢆᣢࡗ࡚࠸ࡿࠖ࡜࠸࠺ࡼࡾࡣᑀࢁ㸪ࠕ୰ᛶỈ⣲ ᰕᐦᗘ NHI ࡀపࡃ Lyǂ ගᏊࡀᢤࡅฟࡋ᫆࠸⎔ቃ࡟࠶ࡿࠖࡇ࡜ࡀ᫂ࡽ࠿࡟࡞ࡗࡓ (Shibuya et al. 2014b)㸬
࠙ࠚᫍ㛫✵㛫࡟࠾ࡅࡿ࢔࣑ࣀ㓟⏕ᡂ࡜ග୙ᩧ໬ࡢ⌮ㄽⓗ◊✲ࠓᏱᐂ࣭⏕࿨ศ㔝㐃ᦠࠔ⏕࿨యࡢᇶᮏศᏊ࡟࢔࣑ࣀ㓟ࡀ࠶ࡿࡀ㸪ᐇ㦂ᐊ࡛࢔࣑ࣀ㓟ࢆసᡂࡍࡿ࡜㸪ᕥᕳࡁ㸦L ᆺ㸧࡜ྑᕳࡁ㸦D ᆺ㸧ࡀྠ㔞⏕ᡂࡉࢀࡿࡀ㸪ᆅ⌫ୖࡢ⏕࿨࡛ࡣᇶᮏⓗ࡟ L ᆺ࢔࣑ࣀ㓟ࡋ࠿౑ࢃࢀ࡚࠸࡞࠸ࠋ
ࡇࢀࢆ㸪㙾ീ␗ᛶయ㐣๫࡜࠸࠺ࠋ1969 ᖺ㸪࣮࢜ࢫࢺࣛࣜ࢔ࡢ࣐࣮ࢳࢯࣥᮧ࡟㝹▼ࡀⴠୗࡋ㸪ࡑࡢ㝹▼࠿ࡽ࢔࣑ࣀ㓟ࡀ᳨ฟࡉࢀࡓࠋࡑࡋ࡚㸪ࢃࡎ࠿࡛ࡣ࠶ࡿࡀ㙾ീ␗ᛶయ㐣๫ࡀⓎぢࡉࢀࡓࠋⓎぢࡉࢀࡓ㙾ീ␗ᛶయ㐣๫ࡣࢃࡎ࠿࡞ࡶࡢ࡛࠶ࡿࡀ㸪ᐇ㦂ࢆࡍࡿ࡜㙾ീ␗ᛶయ㐣๫ࡣ⮬ᕫゐ፹཯ᛂ࡟ࡼࡾᛴ㏿࡟ቑ኱ࡍࡿࡇ࡜ࡀศ࠿ࡗ࡚ࡁࡓࠋࡼࡗ࡚㸪࢔࣑ࣀ㓟ࡢ㙾ീ␗ᛶయ㐣๫ࡀᏱᐂ✵㛫࡛㉳ࡇࡾ㝹▼ࢆ㏻ࡌ࡚ᆅ⌫࡟㐠ࡤࢀ㸪ࡑࢀࡀᆅୖ࡛ᛴ㏿࡟ቑᖜࡋࡓྍ⬟ᛶࡀ࠶ࡿࠋࡲࡓ㸪ᐇ㦂ᐊ࡛෇೫ගࡢගࢆᙜ࡚ࡿ࡜㙾ീ␗ᛶయ㐣๫ࡀᘬࡁ㉳ࡇࡉࢀࡿࡇ࡜ࡀศ࠿ࡗ࡚ࡁࡓࠋࡑࡋ࡚㸪㏆ᖺ࡟࡞ࡗ࡚㸪࢜ࣜ࢜ࣥᗙࡢᫍᙧᡂ㡿ᇦ(OMC-1)ࡸ௚ࡢᫍᙧᡂ㡿ᇦ㸦NGC 6334-V IRN㸧࡛෇೫ගἼࡀⓎぢࡉࢀࡓࠋࡼࡗ࡚㸪ཎጞ⣔ࡢ㏆ࡃ࡛኱㉁㔞ᫍࡀㄌ⏕ࡋࡓ࡜ࡍࢀࡤ㸪ኴ㝧⣔ෆ࡛࢔࣑ࣀ㓟ࡢ㙾ീ␗ᛶయ㐣-42-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩๫ࡀ㉳ࡇࡗࡓྍ⬟ᛶࡀ࠶ࡿࠋ௨ୖࡢ஦ᐇࢆ⫼ᬒ࡟㸪Ᏹᐂ✵㛫࡛෇೫ගἼ࠿ࡽ࢔࣑ࣀ㓟ࡢ㙾ീ␗ᛶయ㐣๫ࢆᘬࡁ㉳ࡇࡍ㐣⛬࡟ࡘ࠸࡚ࡢ㔞Ꮚከయィ⟬ࢆ㐍ࡵ࡚࠸ࡿࠋᡃࠎࡣ㸪෇೫ගἼ྾཰࡜࢔࣑ࣀ
㓟ࡢගບ㉳࡟ࡼࡿᔂቯ࣭ᨵኚ཯ᛂࡢ㐣⛬ࢆゎᯒࡋࡓࠋ➨୍ཎ⌮ィ⟬࡟ࡼࡾ㸪┿✵୰࡟࠾ࡅࡿ࢔࣑
ࣀ㓟ࡢ᭱Ᏻᐃᵓ㐀ࢆồࡵ㸪ࡑࡢග྾཰ᛶ࡜෇೫ග஧Ⰽᛶࡢ್ࢆồࡵࡓࠋࡑࡢ⤖ᯝ㸪࢔࣑ࣀ㓟ࡢග≀ᛶࡣࡑࡢ✀ࡢ≉ᚩ࡜࡞ࡿഃ㙐ࡼࡾ࢔࣑ࣀ㓟඲య࡟ඹ㏻ࡍࡿ୺㙐ࡢᵓ㐀࡟ࡼࡾᙉࡃ౫Ꮡࡋ㸪Ἴ㛗ᖏ࡜ࡋ࡚ࣛ࢖࣐ࣥ ǂ ᖏࡢගࡀ㔜せ࡛࠶ࡿࡇ࡜ࢆ᫂ࡽ࠿࡟ࡋࡓࠋࡲࡓ㸪Ᏹᐂ✵㛫࡟࠾ࡅࡿ࢔࣑ࣀ㓟ࡢ⏕ᡂ࡟ࡘ࠸࡚㸪࢔࣑ࣀ㓟๓㥑యೃ⿵࡛࠶ࡿࣄࢲࣥࢺ࢖ࣥ࠿ࡽ࢔࣑ࣀ㓟࡟⮳ࡿ㐣⛬ࢆ࢚ࢿࣝࢠ࣮
㠃ࡢ㔞ᏊຊᏛィ⟬࡟ࡼࡗ࡚ゎᯒࡋ㸪࢔࣑ࣀࢽࢺࣜࣝࢆ⤒࡚࢔࣑ࣀ㓟ࡀᐜ᫆࡟ᙧᡂࡉࢀᚓࡿࡇ࡜ࡀ
ࢆ♧ࡋࡓࠋ࠙ࠚ⣔እᝨᫍ࡟࠾ࡅࡿගྜᡂ࢔ࣥࢸࢼᶵᵓࡢ◊✲ࠓᏱᐂ࣭⏕࿨ศ㔝㐃ᦠࠔ᥈ᰝᶵ Kepler ࡟ࡼࡗ࡚ኴ㝧⣔እᝨᫍࡢᩘࡣ኱ࡁࡃ㏣ຍࡉࢀ࡚࠾ࡾ, ᆅ⌫ᆺᝨᫍࡸࣁࣅࢱࣈࣝࢰ
࣮ࣥෆ࡟ධࡿᝨᫍࡶⓎぢࡉࢀ࡚࠸ࡿࠋගྜᡂࡣ㸪⏕࿨ࡢ⑞㊧࡛࠶ࡿࣂ࢖࣐࣮࣮࢜࢝ࡢ᭷ຊ࡞ೃ⿵
࡟࡞ࡗ࡚࠸ࡿࠋගྜᡂࡢ⑞㊧ࡢ୰࡛ࡶ 750nm ௜㏆ࡢ㏆㉥እ㡿ᇦ࡟ぢࡽࢀࡿ཯ᑕࢫ࣌ࢡࢺࣝࡢ≉ᚩⓗ࡞໙㓄㸦red edge㸧ࡣࣂ࢖࣐࣮࣮࢜࢝࡜ࡋ࡚㔜せ࡛࠶ࡿࠋᆅ⌫ࡢගྜᡂ⏕≀ࡢሙྜࡣ୺࡛ᫍ࠶
ࡿኴ㝧ࡢࢫ࣌ࢡࢺࣝẚࡢගࢆຠ⋡Ⰻࡃᤕ㞟ࡍࡿࡼ࠺࡟㐍໬ࡋ࡚᮶ࡓ࡜⪃࠼ࡿ࡭ࡁ࡛࠶ࡾ, ࢡࣟࣟࣇ࢕ࣝ࡞࡝ࡢගྜᡂⰍ⣲࠿ࡽ࡞ࡿ࢔ࣥࢸࢼ⣔ࡣ⎔ቃ࡟ࡼࡗ࡚Ⰽ⣲ࡢ✀㢮ࡸ㓄⨨࡞࡝ࡢᙧែࡀ␗࡞
ࡿࠋගࢆཷࡅࡓⰍ⣲ࡣ㟁Ꮚບ㉳ࡉࢀ, ㏆ࡃࡢⰍ⣲࡟㟁Ꮚ≧ែࢆ⛣ືࡉࡏࡿ࡜࠸࠺㐣⛬ࢆ㏻ࡌ࡚ຠ
⋡ⓗ࡟ග࢚ࢿࣝࢠ࣮ࢆ໬Ꮫ࢚ࢿࣝࢠ࣮࡟ኚ᥮ࡍࡿࠋ⣔እᝨᫍ࡟࠾࠸࡚ࡣ␗࡞ࡿගᤕ㞟ࡢᙧែࢆྲྀ
ࡿሙྜ, ࡑࢀ࡟ᑐᛂࡋࡓἼ㛗ᇦ࡟ගྜᡂࡢ඙ೃࢆ♧ࡍྍ⬟ᛶࡀ࠶ࡿࠋᡃࠎࡣ㸪⣔እᝨᫍࡢගࡢࢫ
࣌ࢡࢺࣝẚ࡜᳜≀ࡢගᤕ㞟ࡢᙧែ࡜ࡢ┦㛵࡟ࡘ࠸࡚ᐃ㔞ⓗᣦᶆࢆᑟฟࡍࡿࡇ࡜ࢆ┠ⓗ࡟㸪ගᤕ㞟⣔ࡢ㔞Ꮚ໬Ꮫィ⟬ࢆ⾜ࡗࡓࠋ࢔ࣥࢸࢼࢆᵓᡂࡍࡿⰍ⣲ 1 ࡘ 1 ࡘࡢບ㉳ ≧ែࢆ᫬㛫౫Ꮡᐦᗘỗ㛵ᩘἲ࡟ࡼࡾィ⟬ࡋ, Ⰽ⣲㛫࡛ࡣ཮ᴟᏊ-཮ᴟᏊ┦஫స⏝ࡍࡿ㏆ఝࣔࢹࣝ ࢆᵓ⠏ࡋࡓࠋࡲࡓ, ධᑕග࡜ࡋ࡚࠶ࡿ᣺ືᩘࡢ㟁ሙࢆ༳ຍࡋ࡚⣔ࡢ㔞ᏊຊᏛⓗ᫬㛫Ⓨᒎࢆ㏣㊧ࡍࡿࡇ࡜࡟ࡼࡗ࡚ࢫ࣌ࢡࢺࣝᙉ
ᗘࢆ⟬ฟࡋࡓࠋࡲࡓ㸪࢚ࢿࣝࢠ࣮㍺㏦ຠ⋡ࡀ᭱኱࡜࡞ࡿ୺ᫍࡢ㯮య㍽ᑕᗘࢆồࡵࡓࠋ ᩍ⫱
࠙Ꮫ఩ㄽᩥࠚ
㸺༤ኈㄽᩥ㸼
㸯㸬ᡪ㇂ ㇦
Solving the core-cusp problem of cold dark matter halos and the origin of theirobservational universalities㸰㸬୕ᮌ ὒᖹ
Numerical Investigation of Galactic Merger Utilizing High Performance Computing-43-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩

Architectures: Ancient Satellite Galaxy and Wandering Supermassive Black Hole㸱 㸬 Mohammad Ali Nawaz (The Australian National University, Research School of
Astronomy and Astrophysics)
Interaction of Jets with the Intracluster Medium
㸲㸬Marc White (The Australian National University, Research School of Astronomy andAstrophysics)
Outflows from Young Stellar Objects㸺ಟኈㄽᩥ㸼
㸯㸬᱒ཎ ᓫர▸ᑠ㖟Ἑࡢ⾪✺ࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥ᥈ࡿ㖟Ἑ࡜ࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟࡢෆ㒊ᵓ㐀㸰㸬㕥ᮌ ⿱⾜ෆ㒊⣸እ⥺࡜⫼ᬒ⣸እ⥺ࡀཬࡰࡍ㖟Ἑᙧᡂ࡬ࡢᙳ㡪㸱㸬ᒣ஭ ຬᶞ
࢞ࢫ࡟ࡼࡿຊᏛⓗᦶ᧿ࢆ⪃៖ࡋࡓཎጞ㖟Ἑࣈࣛࢵࢡ࣮࣍ࣝࡢྜయ㐣⛬ࡢ◊✲㸺Ꮫኈㄽᩥ㸼
㸯㸬ᑠᓥ ໶ࣇ࣮ࣜࢻ࣐ࣥ᪉⛬ᘧࡢ᭷㉁㔞ࢽ࣮ࣗࢺࣜࣀ࡟ࡼࡿ⿵ṇ㸰㸬ຍ⸨ ᝆኴᫍ㛫≀㉁࡜㉸᪂ᫍ⇿Ⓨࡢ┦஫స⏝ࡢࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ྥࡅ࡚
㸱㸬ᮌ❧ ె㔛Ᏹᐂࢲࢫࢺୖࡢ࢔࣑ࣀ㓟๓㥑య⏕ᡂ㐣⛬࡜ග୙ᩧ໬ࡢ◊✲㸲㸬㏆⸨ ࡉࡽ࡞  ㉁㔞ኚ໬ࡍࡿ㐃ࣈࣛࢵࢡ࣮࣍ࣝࡢྜయ㐣⛬ࡢ◊✲㸳㸬ᰘ㔝 ⚈ᖹ  CIP ἲ࡟ࡼࡿᩘ್ὶయィ⟬࡟ྥࡅ࡚㸴㸬ྂ㇂ ╎  ☢Ẽᅽຠᯝࢆධࢀࡓࣈࣛࢵࢡ࣮࣍ࣝ㝆╔෇┙ࡢᐃᖖゎ࡟ࡘ࠸࡚ࡢ◊✲㸵㸬⤖ᇛ ᩥ㤶㧗⢭ᗘᏱᐂὶయࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ྥࡅ࡚
࠙㞟୰ㅮ⩏ࠚ࣭ᱵᮧ 㞞அ
ࠕᏱᐂ㍽ᑕὶయຊᏛࡢᇶ♏ࠖ
㸦2013 ᖺ 10 ᭶ 31 ᪥㹼11 ᭶ 1 ᪥㸪ᮾி኱Ꮫᗈᇦࢩࢫࢸ࣒⛉Ꮫ⣔㸪ᮾி㒔㸧 ཷ㈹㸪እ㒊㈨㔠㸪▱ⓗ㈈⏘ᶒ➼࠙ཷ㈹ࠚ⟃Ἴ኱Ꮫᩘ⌮≀㉁⛉Ꮫ◊✲⛉◊✲⛉㛗㈹, ᡪ㇂ ㇦, Solving the core-cusp problem ofcold dark matter halos and the origin of their observational universalities, ᖹᡂ 26 ᖺ3 ᭶ 25 ᪥-44-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩࠙እ㒊㈨㔠ࠚ㸺௦⾲⪅㸼࣭ᇶ┙◊✲㸦㹑㸧㸸ᱵᮧ 㞞அ㸦௦⾲⪅㸧㸦⧞㉺㸧 ࠕ➨୍ୡ௦ኳయ࠿ࡽཎጞ㖟Ἑ࡟⮳ࡿᏱᐂᬯ㯮᫬௦ࡢゎ᫂ࠖ (500 ୓෇)࣭ᇶ┙◊✲㸦㸿㸧㸸᳃ ṇኵ 㸦௦⾲⪅㸧 㸦⧞㉺㸧 ࠕ⌮ㄽ࡜ほࡢ⼥ྜ࡟ࡼࡿ㖟ἙⓎ⏕Ꮫࡢ᥈ồࠖ (150 ୓෇)࣭ᇶ┙◊✲㸦㹁㸧㸸᳃ ṇኵ 㸦௦⾲⪅㸧 㸦᪂つ㸧 ࠕ㍽ᑕὶయࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ࡼࡿ㖟Ἑ⣔⤫ᶞࡢᵓ⠏ࠖ (80 ୓෇)࣭⛉◊㈝ⱝᡭ◊✲㸦㹀㸧㸸⾜᪉ ኱㍜ (௦⾲⪅), 2013-2015 ᖺ, 403 ୓෇ࠕ࣐ࣝࢳࢢ࣮ࣝࣉ㍽ᑕὶయィ⟬࡟ࡼࡿ AGN ࢺ࣮ࣛࢫ࠿ࡽ㝆╔෇┙࡬ࡢ࢞ࢫ౪⤥㐣⛬ࡢゎ࣭᫂ࠖ⛉◊㈝ⱝᡭ◊✲㸦㹀㸧:▼ᒣ ᬛ᫂㸦௦⾲⪅㸧㸪2013-2015 ᖺ㸪350 ୓(3 ᖺ⥲㢠㸪┤᥋⤒㈝)ࠕ㖟Ἑ⣔ෆࡢࢲ࣮ࢡ࣐ࢱ࣮ᚤ⣽ᵓ㐀ࡢゎ᫂࠾ࡼࡧࢲ࣮ࢡ࣐ࢱ᳨࣮ฟ࡬ࡢᛂ⏝࣭ࠖ⛉◊㈝ⱝᡭ◊✲㸦㹀㸧㸸㛗㇂ᕝ ㈼஧㸦௦⾲⪅㸧,

2012 ᖺᗘ᥇ᢥ㸪350 ୓෇ࠕᏱᐂㄽⓗ㍽ᑕࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥゎ᫂ࡍࡿᏱᐂ෌㟁㞳ᮇࡢ㖟Ἑᙧᡂྐࠖ㸺ศᢸ⪅㸼࣭ᡓ␎ⓗ๰㐀◊✲᥎㐍஦ᴗ CREST㸸ᱵᮧ㞞அ㸦ศᢸ⪅㸧㸦௦⾲⪅ ᮔὈ♸㸧ࠕ࣏ࢫࢺ࣌ࢱࢫࢣ࣮ࣝ᫬௦࡟ྥࡅࡓ₇⟬ຍ㏿ᶵᵓ࣭㏻ಙᶵᵓ⤫ྜ⎔ቃࡢ◊✲㛤Ⓨࠖ㸦1188 ୓෇㸧࣭ᣮᡓⓗⴌⱆ◊✲㸸ᱵᮧ㞞அ (ศᢸ⪅)㸦௦⾲⪅㸸㧗ᶫປኴ㸧㸦⥅⥆㸧ࠕ㸴ḟඖගᏊ࣎ࣝࢶ࣐ࣥ᪉⛬ᘧ࡟ࡼࡿ୍⯡┦ᑐㄽⓗ㍽ᑕὶయࢩ࣑࣮ࣗࣞࢩࣙࣥࠖ
㸦10 ୓෇㸧࣭ᇶ┙◊✲㸦㸿㸧㸸ᱵᮧ㞞அ (ศᢸ⪅) 㸦௦⾲⪅㸸኱ෆṇᕭ㸧 㸦⥅⥆㸧ࠕḟୡ௦኱つᶍ᥈ᰝ࡜ࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥᣮࡴᏱᐂ෌㟁㞳ࠖ (1 ୓෇)࣭ᇶ┙◊✲㸦㸿㸧㸸᳃ ṇኵ (ศᢸ⪅) 㸦௦⾲⪅㸸኱ෆṇᕭ㸧 㸦⥅⥆㸧ࠕḟୡ௦኱つᶍ᥈ᰝ࡜ࢩ࣑࣮ࣗࣞࢩ࡛ࣙࣥᣮࡴᏱᐂ෌㟁㞳ࠖ (400 ୓෇)-45-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ ◊✲ᴗ⦼(1) ◊✲ㄽᩥA)

ᰝㄞ௜ࡁㄽᩥ

1)

Miki Y., Mori M., Kawaguchi T., Saito Y., 2014, “Hunting a Wandering
Supermassive Black Hole in the M31 Halo Hermitage”, The Astrophysical Journal,
783, 87-95

2)

Tsuchiya, M., Mori, M., Nitta, S., 2013,“Transonic solutions of isothermal galactic
winds in a cold dark matter halo”, MNRAS, 432, 2837-2845

3)

Miki Y., Takahashi D., Mori M., 2013, “Highly scalable implementation of an N-bodycode on a GPU cluster”, Computer Physics Communications, 184, 2159-21684)

Yuma, S., et al., 2013, “First Systematic Search for Oxygen-line Blobs at HighRedshift: Uncovering AGN Feedback and Star Formation Quenching”, The
Astrophysical Journal, 779, 53-645)

ᡪ㇂ ㇦ , ୕ᮌ ὒᖹ , ᮔ Ὀ♸ , ᳃ ṇኵ , ୰㔛 ┤ே, 2013 ᖺ, ࠕィ⟬Ᏹᐂ≀⌮ࡢࡓࡵࡢ GPU ࢡࣛࢫࢱྥࡅ୪ิ Tree Code ࡢ㛤Ⓨ࡜ᛶ⬟ホ౯ࠖ, ᝟ሗฎ⌮Ꮫ఍ㄽᩥㄅࢥࣥ
ࣆ࣮ࣗࢸ࢕ࣥࢢࢩࢫࢸ࣒㸦ACS㸧, 6(3), 58-706)

Ishiyama, T., et al., 2013, “The Cosmogrid Simulation: Statistical Properties of
Small Dark Matter Halos”, The Astrophysical Journal, 767, 146 (14pp)

7)

Rieder, S., Ishiyama, T., et al., 2013, “Evolution of star clusters in a cosmologicaltidal field”, Monthly Notices of the Royal Astronomical Society, 446, 3695

B)ᰝㄞ↓ࡋㄽᩥ

8)

Kirihara T., Miki Y., Mori M., 2013, “Resolving the outer density profile of dark
matter halo in Andromeda galaxy”, JPhCS, 454, 0120129)

Miki Y., Mori M., Kawaguchi, T., 2013, “Hunting a wandering black hole in M31
halo using GPU cluster”, JPhCS, 454, 012013

10) Ogiya G., Mori M., Miki Y., Boku T., Nakasato N., 2013,“ Studying the core-cusp
problem in cold dark matter halos using N-body simulations on GPU clusters”,
JPhCS, 454, 012014(2) ᅜ㝿఍㆟Ⓨ⾲A) ᣍᚅㅮ₇1) Hasegawa K., “The roles of radiative feedback on galaxies and IGM during the epochof reionization”, Workshop on Photo-Evaporation in Astrophysical Systems(Jun.3-28,
2013, Stockholm, Sweden)2) Wagner, A., Umemura, M., Bicknell, G. V., Sutherland, R., Silk, J., “Mechanical AGN
Feedback - Previous Work and Planned Projects”㸪AGN and Structure Formation
Workshop㸦Jun.20, 2013㸪Institut d'Astrophysique de Paris, France㸧

-46-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩3) Yoshikawa, K., “Vlasov-Poisson Simulations of Astrophysical Self-Gravitating
Systems”, CCS-EPCC Workshop (Jul.4-5, 2013, University of Tsukuba, Japan)4) Wagner, A., Umemura, M., Bicknell, G. V., Sutherland, R., Silk, J., “Feedback in
Galaxy Formation” 㸪 Johns Hopkins University Physics Colloquium (Nov.14,
2013,Johns Hopkins University, Baltimore MD, USA)
5) Wagner, A., Umemura, M., Bicknell, G. V., Sutherland, R., Silk, J., “Galaxy-scale
Feedback by AGN Jets and Winds” 㸪 Workshop on AGN and Starburst-driven
Outflows (Nov.20, 2013, Johns Hopkins University, Baltimore MD, USA)6) ▼ᒣᬛ᫂, “Supercomputer Simulations of Structure Formation in the Universe”,
Taiwan-Japan Symposium on Celestial Mechanics and N-Body Dynamics 2013 (2013ᖺ 12 ᭶ 6 ᪥-8 ᪥,ྎ‴ᅧ❧Ύ⳹኱Ꮵ)7) Yoshikawa, K. “Phantom-GRAPE : High-Performance Library to Accelerate
N-body Calculation with SIMD Instruction Set”, Japan-Korea HPC mini-workshop(Feb. 26-27, 2014, University of Tsukuba, Japan)8) Abe M., Umemura M., Hasegawa K., “Star-cluster formation regulated by theinterstellar radiation field”, Ludwig Maximilians University Munich (Mar.21, 2014,
Munich, Germany)B) ୍⯡ㅮ₇1) Komatsu, Y., Umemura, M., Shoji, M., Yabana, K., Shiraishi, K., Kamiya, K.,
Kayanuma, M., Taguchi, M., Sato, A., “The energy transfer calculation of lightharvesting systems for detecting biomarker on extrasolar planets”, Japan Geoscience
Union Meeting 2013 (May 19-24, 2013, Chiba, Japan)2) Ogiya G., Mori M., “Surfing of dark matter on density waves of galactic gas -Landau
resonance and the core-cusp problem in cold dark matter halos-”, (poster), The
Physical Link between Galaxies and their Halos, Garching by Munich (Jun.24-28,
2013, Germany)3) Igarashi A., Mori M., Nitta S.,“A New Concept of Transonic Galactic Outflows in a
Cold Dark Matter Halo with a Central Super-Massive Black Hole”, The 12th Asia
Pacific Physics Conference (Jul.14-19, 2013, Makuhari, Japan)4) ▼ᒣᬛ᫂,“The formation and evolution of earth-mass dark matter microhalos andtheir impact on indirect probes of dark matter”, Probes of Dark Matter on Galaxy
Scales (Jul. 14-19, 2013, Monterey, USA)-47-

⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩5) Kirihara T., Mori M., Miki Y.,“Andromeda Giant Stream and Outer Density Profile of
the Dark Matter Halo in M31”, (poster), The 12th Asia Pacific Physics Conference(Jul.14-19, 2013, Makuhari, Japan)6) Hasegawa K., “Radiation hydrodynamics simulations on the formation of galaxies
during the epoch of reionization”, (poster), Workshop on Reionization in the Red
Center: New windows on the high redshift Universe (Jul.15-19, 2013, Yulara,
Australia)7) Komatsu, Y., Umemura, M., Shoji, M., Yabana, K., Shiraishi, K., Kamiya, K.,
Kayanuma, M., Sato, A., “The energy transfer simulation for detecting photosynthetic
biosignatures on extrasolar planets”, the 1st Awaji International Workshop on“ Electron Spin Science & Technology ” (Jul.16-18, 2013, Hyogo, Japan)8) Wagner, A., Umemura, M., Bicknell, G. V., Sutherland, R., Silk, J., “Hydrodynamical
Simulations of AGN Feedback”㸪2nd East Asia AGN Workshop㸦Aug.19-23, 2013㸪
Sapporo, Japan㸧9) Shibuya, T.,“A statistical study on galactic outflows of Ly-a emitters probed byvelocity offsets between their Ly-a/UV absorption and nebular lines”, Workshop on
Lyman-alpha as an astrophysical tool (Sep.9-13, 2013, Nordita, Stockholm, Sweden)10)Igarashi A, Mori M. Nitta S.,“Transonic Galactic Outflows and Their Influences to theChemical Evolutions of Galaxies and Intergalactic Space”,(poster),12th International
Symposium on Origin of Matter and Evolution of Galaxies (Nov.18-20, 2013, Tsukuba,
Japan)

11)Komatsu, Y., Umemura, M., Shoji, M., Yabana, K., Shiraishi, K., Kayanuma, M., Sato,A., “Light harvesting and energy transfer in photosystem: implication forbiosignatures”, International Astrobiology Workshop 2013 (Nov.28-30, 2013,
Kanagawa, Japan)

12)Shibuya, T., “Demographics of Lyman Alpha Emitter Structures”, Subaru Users'
Meeting FY2013, NAOJ (Jan.21-23, 2014, Mitaka, Tokyo, Japan)13)Komatsu, Y., Umemura, M., Shoji, M., Shiraishi, K., Kayanuma, M., Yabana, K., Sato,A., “Toward understanding as photosynthetic biosignatures: light harvesting andenergy transfer calculation”, The Search for Life Beyond the Solar System:
Exoplanets, Biosignatures & Instruments (Mar.16-21, 2014, Tuscon, USA)(3) ᅜෆᏛ఍࣭◊✲఍Ⓨ⾲
-48-

⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩A) ᣍᚅㅮ₇1) ᑠᯇຬ,ࠕගྜᡂගᤕ㞟ᶵᵓࡢ㔞Ꮚ໬Ꮫィ⟬࡟ࡼࡿ⣔እᝨᫍࣂ࢖࣐࣮࣮࢜࢝ࡢࣔࢹࣝᵓ
⠏ࠖ,ࠕᏱᐂ࡜⏕࿨ࠖ᠓ヰ఍㸦➨㸯㸱ᅇ㸧㸦2013 ᖺ 6 ᭶ 21 ᪥, ⮬↛⛉Ꮫ◊✲ᶵᵓ᪂ศ㔝๰ᡂࢭࣥࢱ࣮, ᮾி㒔㸧2) Wagner, A., Umemura, M., Bicknell, G. V., SutherlandࠕAGN Feedback by Jetsࠖ㸪Semi-analytic Method with SWANS Meeting㸦 2013 ᖺ 9 ᭶ 19 ᪥㸪࠾ⲔࡢỈዪᏊ኱Ꮫ㸪ᮾி㒔㸧3) ᱵᮧ㞞அ㸪ࠕྂ඾ⓗ෇┙ᙧᡂ㐍໬ ࢩࢼࣜ࢜࡜ၥ㢟Ⅼࠖ㸪෇┙㖟Ἑࡢᙧᡂ࡜㐍໬◊✲఍
㸦2013 ᖺ 9 ᭶ 26 ᪥㹼 28 ᪥㸪ᅜ❧ኳᩥྎ㸪୕㮚ᕷ㸧4) ▼ᒣᬛ᫂㸪ࠕࢫ࣮ࣃ࣮ࢥࣥࣆ࣮ࣗࢱࡢ୰࡛⏕ࡲࢀࡿᏱᐂࠖ,᪥ᮏ≀⌮Ꮫ఍ 2013 ᖺᗘ ኱㜰ᨭ㒊බ㛤ࢩ࣏ࣥࢪ࣒࢘㸦2013 ᖺ 10 ᭶ 26 ᪥, ⏥༡኱Ꮫ, ⚄ᡞᕷ㸧5) ᱵᮧ㞞அ㸪ࠕᏱᐂ⏕࿨ィ⟬⛉Ꮫ㐃ᦠᣐⅬ (CAB) ࡟ࡘ࠸࡚ࠖ㸪ィ⟬ᝨᫍ⛉Ꮫࢩ࣏ࣥࢪ࣒࢘㸪
㸦2013 ᖺ 11 ᭶ 23 ᪥㸪▼ᇉ㞳ᓥࢱ࣮࣑ࢼࣝ㸪▼ᇉᕷ㸧6) ▼ᒣᬛ᫂㸪ࠕ࣌ࢱࣇࣟࢵࣉࢫ⣭ N యࢩ࣑࣮ࣗࣞࢱࡢ㛤Ⓨ Ɇࢲ࣮ࢡ࣐ࢱ࣮ࡢ㉸኱つᶍࢩ࣑࣮ࣗࣞࢩࣙࣥɆࠖ,ࠕிࠖ࡟࠾ࡅࡿ㧗㏿໬࣮࣡ࢡࢩࣙࢵࣉ㸦2013 ᖺ 12 ᭶ 18 ᪥, ⌮໬Ꮫ◊✲ᡤィ⟬⛉Ꮫ◊✲ᶵᵓ㸪⚄ᡞᕷ㸧7) ྜྷᕝ⪔ྖ㸪ࠕ⾪✺㖟Ἑᅋ࡟࠾ࡅࡿ㠀ᖹ⾮㟁㞳㐣⛬࡜஧ᗘᵓ㐀ࠖ,ࠕ㖟Ἑᅋࡢ≀⌮ࠖ◊✲఍㸪㸦2013 ᖺ 12 ᭶ 28 ᪥, ᮾி⌮⛉኱Ꮫ⚄ᴦᆏ࢟ࣕࣥࣃࢫ㸪ᮾி㒔㸧8) 㛗㇂ᕝ㈼஧ 㸪
ࠕ㏆ᖺࡢᏱᐂ෌㟁㞳࡟㛵ࡍࡿ⌮ㄽ࣭ほ◊✲ࡢ㐍ᒎ࡜௒ᚋࡢㄢ㢟ࠖ㸪ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍㸦2014 ᖺ 1 ᭶ 22 ᪥㹼24 ᪥, 㮵ඣᓥ኱Ꮫ, 㮵ඣᓥᕷ㸧9) ᱵᮧ㞞அ㸪ࠕᏱᐂ⏕࿨ィ⟬⛉Ꮫ㐃ᦠᣐⅬࡢ㐍ࡵ᪉࡟ࡘ࠸࡚ࠖ
㸪◊✲఍ࠕᆅୖᐇ㦂࣭Ᏹᐂᐇ㦂࣭ほ࣭ィ⟬ࢩࢼࢪ࣮࡟ࡼࡿᫍ㛫࡛ࡢ⏕యศᏊ࣭⏕యᶵ⬟๰⏕ࡢゎ᫂ࠖ㸦2014 ᖺ 2 ᭶

3 ᪥, ⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮㸪ࡘࡃࡤᕷ㸧10) 㛗㇂ᕝ㈼஧㸪ࠕ෌㟁㞳ࢩ࣑࣮ࣗࣞࢩࣙࣥࠖ㸪ࠕ㖟Ἑ㐍໬࡜㐲᪉Ᏹᐂࠖ◊✲఍㸦2014 ᖺ 3 ᭶
24 ᪥㹼25 ᪥, ᮾி኱Ꮫᮏ㒓࢟ࣕࣥࣃࢫ㸪ᮾி㒔)B) ࡑࡢ௚ࡢⓎ⾲1) ᱵᮧ㞞அ㸪ࠕᏱᐂ⏕࿨ィ⟬⛉Ꮫ㐃ᦠᣐⅬ࡟ࡘ࠸࡚ࠖ㸪ࠕᏱᐂ⏕࿨ィ⟬⛉Ꮫ㐃ᦠᣐⅬ࣮ࠖ࣡ࢡࢩࣙࢵࣉ㸦2013 ᖺ 6 ᭶ 28 ᪥㹼29 ᪥㸪⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮㸪ࡘࡃࡤᕷ㸧2) ஬༑ᔒᮒኟ, ᳃ṇኵ, ᪂⏣ఙஓ, ࠕ⌫ᑐ⛠ᐃᖖ㖟Ἑ㢼ᶍᆺ࡟ࡼࡿ Sombrero 㖟Ἑࡢ X ⥺ᙉᗘศᕸࠖ, ᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10 ᪥㹼12 ᪥, ᮾ໭኱Ꮫ, ௝ྎᕷ㸧3) ஬༑ᔒᮒኟ, ᳃ṇኵ, ᪂⏣ఙஓ, ࠕࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟ࡜㖟Ἑ୰ᚰࣈࣛࢵࢡ࣮࣍ࣝࡢ㔜ຊሙ࡟࠾ࡅࡿ⌫ᑐ⛠ᐃᖖ㖟Ἑ㢼ゎᯒࠖ, ᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10-49-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩᪥㹼12 ᪥, ᮾ໭኱Ꮫ, ௝ྎᕷ㸧4) ▼ᒣᬛ᫂,ࠕ᭱ᑠࢫࢣ࣮ࣝ࠿ࡽࡣࡌࡲࡿ㝵ᒙⓗࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟᙧᡂࠖ,᪥ᮏኳᩥᏛ఍
2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10 ᪥㹼12 ᪥, ᮾ໭኱Ꮫ, ௝ྎᕷ㸧5) ᡪ㇂㇦㸪᳃ṇኵ㸪▼ᒣᬛ᫂㸪Andreas Burkert㸪ࠕࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟࡢ㉁㔞ᐦᗘᵓ㐀࠿ࡽ᥈ࡿほⓗ⤒㦂๎ࠖ㸪᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10 ᪥㹼12 ᪥, ᮾ໭኱Ꮫ, ௝ྎᕷ㸧6) ᑠᯇຬ, ᱵᮧ㞞அ, ᗉྖග⏨, ▮ⰼ୍ᾈ, ⓑ▼㈼஧, ⚄㇂ඞᨻ, ᰰ἟ឡ, బ⸨ⓡඔ, ࠕ⣔እᝨᫍ࡟࠾ࡅࡿගྜᡂࡢ⑞㊧ࡢᣦᶆᵓ⠏ࡢࡓࡵࡢගᤕ㞟ィ⟬ࠖ, ᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍, 㸦2013 ᖺ 9 ᭶ 10 ᪥ࠥ12 ᪥, ᮾ໭኱Ꮫ, ௝ྎᕷ㸧7) 㕥ᮌ⿱⾜㸪ᱵᮧ㞞அ㸪ࠕෆ㒊⣸እ⥺࣭⫼ᬒ⣸እ⥺ࡀཬࡰࡍ㖟Ἑ㐍໬࡬ࡢᙳ㡪ࠖ,᪥ᮏኳᩥ
Ꮫ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10 ᪥㹼12 ᪥, ᮾ໭኱Ꮫ, ௝ྎᕷ㸧8) ⏣୰㈼, ྜྷᕝ⪔ྖ, ᒸᮏᓫ, 㛗㇂ᕝ㈼஧,ࠕGPU ࢆ⏝࠸ࡓ㍽ᑕ㍺㏦ࢩ࣑࣮ࣗࣞࢩࣙࣥࡢ㧗㏿໬ࠖ,᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10 ᪥㹼12 ᪥㸪ᮾ໭኱Ꮫ㸪௝ྎᕷ㸧9) 㛗㇂ᕝ㈼஧ , ࠕ⣸እ⥺ࣇ࢕࣮ࢻࣂࢵࢡࡀ෌㟁㞳ᮇࡢ㖟Ἑࡸ㖟Ἑ㛫≀㉁࡟୚࠼ࡿᙳ㡪ࠖ, ᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦2013 ᖺ 9 ᭶ 10 ᪥㹼12 ᪥㸪ᮾ໭኱Ꮫ㸪௝ྎᕷ㸧10) Wagner, A., Umemura, M., Bicknell, G. V., Sutherland, R., Silk, J.,ࠕKinetic-mode
Feedback: Radio Galaxies and UFOsࠖ㸪᪥ᮏኳᩥᏛ఍ 2013 ᖺ⛅Ꮨᖺ఍㸦 2013 ᖺ 9 ᭶
10 ᪥㹼12 ᪥㸪ᮾ໭኱Ꮫ㸪௝ྎᕷ㸧11) ஬༑ᔒᮒኟ, ᳃ṇኵ, ᪂⏣ఙஓ,ࠕ㖟Ἑ୰ᚰࣈࣛࢵࢡ࣮࣍ࣝ࡜ࢥ࣮ࣝࢻࢲ࣮ࢡ࣐ࢱ࣮ࣁࣟ
࣮ࡢ㔜ຊሙ࡟࠾ࡅࡿ㑄㡢㏿㖟㢼ゎᯒ࡜ࡑࡢᛂ⏝ࠖ, ὶయຊᏛ఍㸦2013 ᖺ 9 ᭶ 12 ᪥㹼14᪥㸪ᮾி㎰ᕤ኱Ꮫ㸪ᗓ୰ᕷ㸧12) ᱵᮧ㞞அ㸪ࠕ㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝᙧᡂ㸸㝆╔ vs ྜయࠖ㸪㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ◊✲᥎㐍㐃⤡఍࣭࢟ࢵࢡ࢜ࣇ࣮࣡ࢡࢩࣙࢵࣉ㸦2013 ᖺ 9 ᭶ 16 ᪥㹼17 ᪥㸪ឡ፾኱Ꮫ㸪ᯇᒣᕷ㸧13) ୕ᮌὒᖹ㸪᳃ṇኵ㸪ᕝཱྀಇᏹ㸪⃽⸨♸⌮Ꮚ㸪ࠕ኱つᶍ GPU ࢡࣛࢫࢱࢆ㥑౑ࡋࡓ M31 ࣁ࣮ࣟࢆ⁻࠺ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ᥈ᰝࠖ㸪㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ◊✲᥎㐍㐃⤡఍࣭࢟ࢵࢡ࢜
ࣇ࣮࣡ࢡࢩࣙࢵࣉ㸦2013 ᖺ 9 ᭶ 16 ᪥㹼17 ᪥㸪ឡ፾኱Ꮫ㸪ᯇᒣᕷ㸧14) ᱵᮧ㞞அ㸪ࠕᏱᐂὶయࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ࡼࡿኳయᙧᡂࡢ◊✲ࠖ㸪➨㸳ᅇࠕᏛ㝿ィ⟬⛉Ꮫ࡟ࡼࡿ᪂ࡓ࡞▱ࡢⓎᒎ࣭⤫ྜ࣭๰ฟࠖࢩ࣏ࣥࢪ࣒࢘ 㸫T2K-TsukubaࠊHA-PACS ࡟ࡼࡿィ⟬⛉ᏛࡢⓎᒎ࡜ࠊḟୡ௦ࢥࣥࣆ࣮ࣗࢸ࢕ࣥࢢࡢᒎᮃ㸫㸦2013 ᖺ 11 ᭶ 5 ᪥㹼6 ᪥㸪⟃Ἴ኱Ꮫ㸪ࡘࡃࡤᕷ㸧15) ᱵᮧ㞞அ㸪ࠕᏱᐂ⏕࿨ィ⟬⛉Ꮫ㐃ᦠ࡟ࡘ࠸࡚ࠖ㸪⮬↛⏺࡟࠾ࡅࡿ⏕యศᏊ࢟ࣛࣜࢸ࢕㉳※㸫ᐇ㦂࣭ほ࣭ィ⟬ࢩࢼࢪ࣮࡟ࡼࡿ࢔ࣉ࣮ࣟࢳ㸦2013 ᖺ 11 ᭶ 16 ᪥㸪ᒸᓮࢥࣥࣇ࢓ࣞ

ࣥࢫࢭࣥࢱ࣮㸧-50-

⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩16) ᑠᯇຬ, ࠕ ⣔እᝨᫍࡢࣂ࢖᳨࣐࣮࣮࢜࢝ウ࡟ྥࡅ࡚㸸ගྜᡂࡢග྾཰ࣔࢹࣝࠖ, ALMA࣮࣡ࢡࢩࣙࢵࣉࠕᏱᐂ࡜⏕࿨ࠖ㸦2013 ᖺ 11 ᭶ 23 ᪥, ᅜ❧ኳᩥྎ㸪୕㮚ᕷ㸧17) Ᏻ㒊∾ே㸪ᱵᮧ㞞அ㸪㛗㇂ᕝ㈼஧㸪ࠕᫍ㛫㍽ᑕሙ࡟ࡼࡗ࡚ไᚚࡉࢀࡿᫍᅋᙧᡂ㐣⛬ࡢ 3ḟඖ㍽ᑕὶయຊᏛ࡟ࡼࡿ◊✲ࠖ㸪➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘㸦2013 ᖺ 12 ᭶ 25 ᪥㹼27
᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃࢫ, ᯽ᕷ㸧18) ஬༑ᔒᮒኟ, ᳃ṇኵ, ᪂⏣ఙஓ, ࠕ㑄㡢㏿㖟Ἑ㢼ࡀ㖟Ἑ㛫✵㛫ࡢ໬Ꮫ㐍໬࡟୚࠼ࡿᙳ㡪ࠖ,➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘㸦2013 ᖺ 12 ᭶ 25 ᪥㹼27 ᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃࢫ, ᯽ᕷ㸧19) ᡪ㇂㇦㸪ࠕࢥ࣮ࣝࢻࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟࡢࢥ࢔-࢝ࢫࣉၥ㢟ࡢゎỴ࡜ࡑࡢほⓗ⤒㦂๎ࡢ㉳※ࠖ㸪➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘㸦2013 ᖺ 12 ᭶ 25 ᪥㹼27 ᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃ
ࢫ, ᯽ᕷ㸧
20) ᱒ཎᓫர, ୕ᮌὒᖹ, ᕝཱྀಇᏹ, ᳃ṇኵ, ࠕ࢔ࣥࢻ࣓ࣟࢲࢫࢺ࣮࣒ࣜ࡜ẕ▸ᑠ㖟Ἑࡢෆ㒊ᵓ㐀ࠖ, (࣏ࢫࢱ࣮), ➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘㸦2013 ᖺ 12 ᭶ 25 ᪥㹼27 ᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃࢫ, ᯽ᕷ㸧21) ⾜᪉኱㍜, ᱵᮧ㞞அ, 㛗㇂ᕝ೺஧, ࠕAGN ࡢ㍽ᑕ࡟ࡉࡽࡉࢀࡓศᏊ㞼ࡢᑑ࿨ࠖ, (࣏ࢫࢱ࣮)㸪➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘ 㸦2013 ᖺ 12 ᭶ 25 ᪥㹼27 ᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃࢫ,᯽ᕷ㸧22) 㛗㇂ᕝ㈼஧, ࠕᏱᐂ෌㟁㞳㐣⛬࡟࠾ࡅࡿ㍽ᑕᛶࣇ࢕࣮ࢻࣂࢵࢡࡢ㔜せᛶࠖ, 㸦࣏ࢫࢱ࣮㸧㸪➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘㸦2013 ᖺ 12 ᭶ 25 ᪥㹼27 ᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃࢫ, ᯽ᕷ㸧23) ୕ᮌὒᖹ㸪᳃ṇኵ㸪ᕝཱྀಇᏹ㸪⃽⸨♸⌮Ꮚ㸪ࠕNumerical Investigation of Merger
Remnants Utilizing High Performance Computing Architectures: Ancient Satellite
Galaxy and Wandering Supermassive Black Holeࠖ㸪➨ 26 ᅇ⌮ㄽ᠓ࢩ࣏ࣥࢪ࣒࢘㸦2013ᖺ 12 ᭶ 25 ᪥㹼27 ᪥, ᮾி኱Ꮫ᯽࢟ࣕࣥࣃࢫ, ᯽ᕷ㸧24) Ᏻ㒊∾ே, ᱵᮧ㞞அ, 㛗㇂ᕝ㈼஧㸪ࠕᫍ㛫㍽ᑕሙ࡟ࡼࡗ࡚ไᚚࡉࢀࡿᫍᅋᙧᡂ㐣⛬ࡢ 3 ḟ
ඖ㍽ᑕὶయຊᏛ࡟ࡼࡿ◊✲ࠖ㸪ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍㸦2014 ᖺ 1 ᭶ 22 ᪥ࠥ24 ᪥㸪㮵ඣᓥ኱Ꮫ㸪㮵ඣᓥᕷ㸧25) ஬༑ᔒᮒኟ, ᳃ṇኵ, ᪂⏣ఙஓ, ࠕࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟ࡜㖟Ἑ୰ᚰࣈࣛࢵࢡ࣮࣍ࣝࡢ㔜ຊሙ࡟࠾ࡅࡿ⌫ᑐ⛠ᐃᖖ㖟Ἑ㢼ゎᯒࠖ, ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍㸦2014 ᖺ 1 ᭶ 22 ᪥㹼24᪥, 㮵ඣᓥ኱Ꮫ㸪㮵ඣᓥᕷ㸧26) ▼ᒣᬛ᫂,ࠕ᭱ᑠࡢࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟ࠿ࡽࡢ㝵ᒙⓗᵓ㐀ᙧᡂࠖ, CfCA ࣮ࣘࢨ࣮ࢬ࣑࣮ࢸ
࢕ࣥࢢ㸦2014 ᖺ 1 ᭶ 28 ᪥㹼29 ᪥㸪ᅜ❧ኳᩥྎ୕㮚࢟ࣕࣥࣃࢫ㸪୕㮚ᕷ㸧27) ⾜᪉኱㍜, ᱵᮧ㞞அ, 㛗㇂ᕝ೺஧, ࠕAGN ࡢ㍽ᑕ࡟ࡉࡽࡉࢀࡓ࢞ࢫ㞼ࡢ㍽ᑕὶయィ⟬ࠖ,ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍ 㸦2014 ᖺ 1 ᭶ 22 ᪥㹼24 ᪥, 㮵ඣᓥ኱Ꮫ, 㮵ඣᓥᕷ㸧28) 㕥ᮌ⿱⾜㸪ᱵᮧ㞞அ,ࠕෆ㒊ཬࡧ⫼ᬒ⣸እ⥺࡟ࡼࡿ㖟Ἑࡢᫍᙧᡂྐ࡬ࡢᙳ㡪ࠖ, ึ௦࣭ᫍ-51-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ึ௦㖟Ἑ◊✲఍㸦2014 ᖺ 1 ᭶ 22 ᪥ࠥ24 ᪥㸪㮵ඣᓥ኱Ꮫ㸪㮵ඣᓥᕷ㸧29) ᱵᮧ㞞அ,ࠕࡲ࡜ࡵࠖ㸪ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍㸦2014 ᖺ 1 ᭶ 22 ᪥ࠥ24 ᪥㸪㮵ඣᓥ኱Ꮫ㸪㮵ඣᓥᕷ㸧30) ᒣ஭ຬᶞ, ࠕ࢞ࢫ࡟ࡼࡿຊᏛⓗᦶ᧿ࢆ⪃៖ࡋࡓཎጞ㖟Ἑࣈࣛࢵࢡ࣮࣍ࣝࡢྜయ㐣⛬ࡢ◊✲ࠖ, ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍㸦2014 ᖺ 1 ᭶ 22 ᪥㹼24 ᪥㸪㮵ඣᓥ኱Ꮫ㸪㮵ඣᓥᕷ㸧31) ⾜᪉኱㍜, ᱵᮧ㞞அ, 㛗㇂ᕝ㈼஧, ࠕAGN ࡢ㍽ᑕ࡟ࡉࡽࡉࢀࡓศᏊ㞼ࡢᑑ࿨ࠖ, (࣏ࢫࢱ࣮)㸪 ᅜ❧ኳᩥྎ CfCA ࣮ࣘࢨ࣮ࢬ࣑࣮ࢸ࢕ࣥࢢ㸦2014 ᖺ 1 ᭶ 28 ᪥㹼29 ᪥㸪ᅜ❧ኳᩥྎ୕㮚࢟ࣕࣥࣃࢫ㸪୕㮚ᕷ㸧32) 㛗㇂ᕝ㈼஧㸪ࠕᏱᐂㄽⓗ㍽ᑕὶయィ⟬࡛ゎ᫂ࡍࡿ෌㟁㞳ᮇࡢᏱᐂ㐍໬ྐࠖ㸪 (࣏ࢫࢱ࣮)㸪
ᅜ❧ኳᩥྎ CfCA ࣮ࣘࢨ࣮ࢬ࣑࣮ࢸ࢕ࣥࢢ㸦2014 ᖺ 1 ᭶ 28 ᪥㹼29 ᪥㸪ᅜ❧ኳᩥྎ୕㮚࢟ࣕࣥࣃࢫ㸪୕㮚ᕷ㸧33) ྜྷᕝ⪔ྖ,ࠕVlasov ࢩ࣑࣮ࣗࣞࢩࣙࣥ࡟ࡼࡿᏱᐂ኱つᶍᵓ㐀ᙧᡂ࡟࠾ࡅࡿࢽ࣮ࣗࢺࣜࣀࡢ
ࢲ࢖ࢼ࣑ࢡࢫࠖ, ᅜ❧ኳᩥྎ CfCA ࣮ࣘࢨ࣮ࢬ࣑࣮ࢸ࢕ࣥࢢ㸦2014 ᖺ 1 ᭶ 28 ᪥㹼29 ᪥㸪ᅜ❧ኳᩥྎ୕㮚࢟ࣕࣥࣃࢫ㸪୕㮚ᕷ㸧34) ஬༑ᔒᮒኟ㸪᳃ṇኵ㸪᪂⏣ఙஓ, ࠕࢲ࣮ࢡ࣐ࢱ࣮ࣁ࣮ࣟ࡜㖟Ἑ୰ᚰࣈࣛࢵࢡ࣮࣍ࣝࡢ㔜ຊሙ࡟࠾ࡅࡿ⌫ᑐ⛠ᐃᖖ㖟Ἑ㢼ゎᯒࠖ㸪ࣉࣛࢬ࣐ࢭ࣑ࢼ࣮㸦2014 ᖺ 1 ᭶ 31 ᪥㸪୕㮚ᕷ㸧35) ᑠᯇຬ, ࠕගྜᡂࡢග྾཰ィ⟬㸸ኴ㝧⣔እᝨᫍࡢࣂ࢖࣐࣮࣮࢜࢝࡬ࡢ♧၀ࠖ, ᆅୖᐇ㦂࣭Ᏹᐂᐇ㦂࣭ほ ࣭ィ⟬ࢩࢼࢪ࣮࡟ࡼࡿᫍ㛫࡛ࡢ⏕యศᏊ࣭⏕యᶵ⬟๰⏕ࡢゎ᫂㸦2014 ᖺ
2 ᭶ 3 ᪥, ⟃Ἴ኱Ꮫ㸪ࡘࡃࡤᕷ㸧36) 㛗㇂ᕝ㈼஧㸪ࠕᏱᐂึᮇࡢ㖟Ἑᙧᡂ࡜Ᏹᐂ෌㟁㞳ࠖ,HPCI ᡓ␎ࣉࣟࢢ࣒ࣛศ㔝 5ࠕ≀㉁࡜
Ᏹᐂࡢ㉳※࡜ᵓ㐀ࠖ඲యࢩ࣏ࣥࢪ࣒࢘㸦2014 ᖺ 3 ᭶ 3 ᪥㹼4 ᪥㸪ᐩኈࢯࣇࢺࣉࣛࢨ㸪ᮾி㒔㸧37) Ᏻ㒊∾ே㸪ᱵᮧ㞞அ㸪ࠕᫍ㛫㍽ᑕሙ࡟ࡼࡗ࡚ไᚚࡉࢀࡿᫍᅋᙧᡂ㐣⛬ࡢ 3 ḟඖ㍽ᑕὶయຊᏛ࡟ࡼࡿ◊✲ࠖ㸪᪥ᮏኳᩥᏛ఍᫓Ꮨᖺ఍㸦2014 ᖺ 3 ᭶ 19 ᪥ࠥ22 ᪥㸪ᅜ㝿ᇶ╩ᩍ኱Ꮫ㸪୕㮚ᕷ㸧38) ᱒ཎᓫர, ୕ᮌὒᖹ, ᳃ṇኵ, ᕝཱྀಇᏹ, ࠕ࢔ࣥࢻ࣓ࣟࢲࢫࢺ࣮࣒࡛ࣜ᥈ࡿẕ▸ᑠ㖟Ἑࡢෆ㒊ᵓ㐀ࠖ, ᪥ᮏኳᩥᏛ఍ 2014 ᖺ᫓Ꮨᖺ఍㸦2014 ᖺ 3 ᭶ 19 ᪥㹼22 ᪥㸪ᅜ㝿ᇶ╩ᩍ኱Ꮫ, ୕㮚ᕷ㸧39) ⃅㇂㝯ಇ, ࠕLyǂ ㍤⥺㖟Ἑࡢ㏿ᗘᵓ㐀◊✲࡛᥈ࡿ Lyǂ ࡢᨺᑕᶵᵓࠖ,᪥ᮏኳᩥᏛ఍᫓Ꮨ
ᖺ఍ 㸦2014 ᖺ 3 ᭶ 19 ᪥ࠥ22 ᪥, ᅜ㝿ᇶ╩ᩍ኱Ꮫ㸪୕㮚ᕷ㸧40) ⾜᪉኱㍜, ᱵᮧ㞞அ, 㛗㇂ᕝ㈼஧, ࠕAGN ࡢ㍽ᑕ࡟ࡉࡽࡉࢀࡓ࢞ࢫ㞼ࡢ㍽ᑕὶయィ⟬II.ࠖ, ᪥ᮏኳᩥᏛ఍᫓Ꮨᖺ఍ 㸦2014 ᖺ 3 ᭶ 19 ᪥㹼22 ᪥, ᅜ㝿ᇶ╩ᩍ኱Ꮫ, ୕㮚ᕷ㸧-52-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩41) ୕ᮌὒᖹ㸪᳃ṇኵ㸪ᕝཱྀಇᏹ㸪ࠕ኱つᶍ GPU ࢡࣛࢫࢱࢆ⏝࠸࡚᥈ࡿ M31 ࣁ࣮ࣟࢆ⁻࠺㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝࡢ⌧ᅾ఩⨨ࠖ㸪᪥ᮏኳᩥᏛ఍ 2014 ᖺ᫓Ꮨᖺ఍㸦2014 ᖺ 3 ᭶ 19 ᪥
㹼22 ᪥㸪ᅜ㝿ᇶ╩ᩍ኱Ꮫ, ୕㮚ᕷ㸧42) Wagner, A., Umemura, M., Bicknell, G. V., Sutherland, R., Silk, J.ࠕPositive vsNegative AGN Feedback in Galaxy FormationࠖSemi-analytic Method with SWANS
Workshop㸦2014 ᖺ 3 ᭶ 27 ᪥㹼28 ᪥㸪⌮໬Ꮫ◊✲ᡤィ⟬⛉Ꮫ◊✲ᶵᵓ㸪⚄ᡞᕷ㸧(4) ⴭ᭩㸪ゎㄝグ஦➼ᱵᮧ㞞அࢩ࣮ࣜࢬ㸺Ᏹᐂ≀⌮Ꮫࡢᇶ♏㸼ձࠕᏱᐂὶయຊᏛࡢᇶ♏ࠖ㸪⚟Ụ⣧㸪࿴⏣᱇୍㸪ᱵᮧ㞞அⴭ㸦᪥ᮏホㄽ♫ 㸪2014 ᖺ 2 ᭶㸧 ␗ศ㔝㛫㐃ᦠ࣭ᅜ㝿㐃ᦠ࣭ᅜ㝿άື➼࠙␗ศ㔝㛫㐃ᦠࠚ1)

ᫍ㛫࢔࣑ࣀ㓟 L ᆺ㐣๫ࡢ◊✲㸦ᱵᮧ㸪ᮌ❧㸧Ᏹᐂ࣭⏕࿨ศ㔝㛫㐃ᦠ࡟ࡼࡾ㸪࢔࣑ࣀ㓟๓㥑య࠿ࡽࡢ࢔࣑ࣀ㓟⏕ᡂ㸪࠾ࡼࡧ෇೫ගἼ↷ᑕ࡟ࡼࡿ࢔࣑ࣀ㓟㙾ീ␗ᛶయ㐣๫࡟ࡘ࠸࡚ࡢ㔞ᏊຊᏛィ⟬ࢆ㐍ࡵࡓࠋ2) ⣔እᝨᫍ࡟࠾ࡅࡿගྜᡂ࢔ࣥࢸࢼᶵᵓࡢ◊✲㸦ᑠᯇ㸪ᱵᮧ㸧Ᏹᐂ࣭⏕࿨ศ㔝㛫㐃ᦠ࡟ࡼࡾ㸪⣔እᝨᫍ⣔ࡢ୺ᫍගࢫ࣌ࢡࢺࣝ࡜ගྜᡂගᤕ㞟ࡢ┦㛵࡟ࡘ࠸࡚㔞Ꮚ໬Ꮫィ⟬ࢆ㐍ࡵࡓࠋ࠙ᅜ㝿㐃ᦠࠚ
࣭Alex Wagner
Collaboration with Prof. Joseph Silk (IAP) and Prof. Colin Norman on "Positive Feedback
through AGN-pressure Induced Star Formation in Disk Galaxies." Visiting researcher tothe Institut d'Astrophysique de Paris, France, and Johns Hopkins University, BaltimoreMD.

 ࢩ࣏ࣥࢪ࣒࢘㸪◊✲఍㸪ࢫࢡ࣮ࣝ➼ࡢ㛤ദᐇ⦼㸯㸧ࠕᏱᐂ⏕࿨ィ⟬⛉Ꮫ㐃ᦠᣐⅬ࣮ࠖ࣡ࢡࢩࣙࢵࣉ

 2013 ᖺ 6 ᭶ 28 ᪥㹼29 ᪥㸪⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮㸪ࡘࡃࡤᕷ㸰㸧㉸ᕧ኱ࣈࣛࢵࢡ࣮࣍ࣝ◊✲᥎㐍㐃⤡఍࣭࢟ࢵࢡ࢜ࣇ࣮࣡ࢡࢩࣙࢵࣉ

2013 ᖺ 9 ᭶ 16 ᪥㹼17 ᪥㸪ឡ፾኱Ꮫ⌮Ꮫ㒊㸪ᯇᒣᕷ㸱㸧෇┙㖟Ἑࡢᙧᡂ࡜㐍໬◊✲఍

-53-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩ 2013 ᖺ 9 ᭶ 26 ᪥㹼28 ᪥㸪ᅜ❧ኳᩥྎ㸪୕㮚ᕷ㸲㸧ኳయᙧᡂ◊✲఍

 2013 ᖺ 10 ᭶ 4 ᪥㹼5 ᪥㸪⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮㸪ࡘࡃࡤᕷ㸳㸧ࠕほ࡜⌮ㄽ࡛᥈ࡿᏱᐂ෌㟁㞳࡜㐲᪉㖟Ἑᙧᡂ࣮ࠖ࣡ࢡࢩࣙࢵࣉ

2013 ᖺ 11 ᭶ 27 ᪥㹼29 ᪥㸪⚄ᡞ኱Ꮫ㸪⚄ᡞᕷ㸴㸧ᅜ㝿఍㆟ࠕ2nd East Asian AGN Workshop in Sapporoࠖ
㸪2013 ᖺ 8 ᭶ 19 ᪥㹼23 ᪥㸪ࣈ࣮࢙࣮ࣝ࢘ࣈ࢖ࣥᮐᖠᕷ㸦http://www.kusastro.kyoto-u.ac.jp /~matsuoka/20130312agnw㸧
㸵㸧ึ௦࣭ᫍึ௦㖟Ἑ◊✲఍ 20142014 ᖺ 1 ᭶ 22 ᪥㹼24 ᪥㸪㮵ඣᓥ኱Ꮫ⌮Ꮫ㒊㸪㮵ඣᓥᕷ ⟶⌮࣭㐠Ⴀ࣭ᱵᮧ㞞அィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ ࢭࣥࢱ࣮㛗ィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ 㐠Ⴀጤဨ఍ጤဨ㛗ィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ ே஦ጤဨ఍ጤဨ㛗ィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ Ᏹᐂ࣭ཎᏊ᰾≀⌮◊✲㒊㛛୺௵ィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ 㐠Ⴀ༠㆟఍ጤဨィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ ◊✲௻⏬ᐊጤဨ≀⌮Ꮫᇦ 㐠Ⴀጤဨ఍ጤဨ
≀⌮Ꮫᇦ Ᏹᐂ≀⌮⌮ㄽࢢ࣮ࣝࣉ㛗≀⌮Ꮫ㢮 Ꮫົጤဨ㸪࣒࢝ࣜ࢟ࣗࣛጤဨ఍ጤဨ㛗ᮾிᕤᴗ኱ᏛࠕGCOE ᆅ⌫࠿ࡽᆅ⌫ࡓࡕ࡬ࠖእ㒊ホ౯ጤဨ࣭ྜྷᕝ⪔ྖィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮࣭ィ⟬ᶵ㐠⏝ጤဨィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮࣭࣓ࢽ࣮ࢥ࢔ᆺ኱つᶍࢫ࣮ࣃ࣮ࢥࣥࣆ࣮ࣗࢱࢩࢫࢸ࣒௙ᵝ⟇ᐃጤဨ఍࣭ጤဨィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮࣭኱つᶍ࣓ࢽ࣮ࢥ࢔ᐇ㦂ࢩࢫࢸ࣒௙ᵝ⟇ᐃጤဨ఍࣭ጤဨ
ィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮࣭ᐦ⤖ྜ୪ิ₇⟬ຍ㏿ᶵᵓᐇ㦂ࢩࢫࢸ࣒௙ᵝ⟇ᐃጤဨ఍࣭ጤဨ

♫఍㈉⊩࣭ᅜ㝿㈉⊩࣭ྜྷᕝ⪔ྖࠕᏱᐂ኱つᶍᵓ㐀 㸫Ᏹᐂࡣ⣲⢏Ꮚࡢክࢆぢࡿ࠿㸫ࠖ㸪඲ᅜྠ᫬୐ኤㅮ₇఍ 2013㸦2013 ᖺ 7 ᭶-54-⟃Ἴ኱Ꮫィ⟬⛉Ꮫ◊✲ࢭࣥࢱ࣮ᖹᡂ  ᖺᗘᖺḟሗ࿌᭩

6 ᪥㸪ࡘࡃࡤᅜ㝿఍㆟ሙ㸪ࡘࡃࡤᕷ㸧
࣭Alex Wagner
Publication of a free, open-source code to create initial conditions representative of afractal, log-normal, inter-stellar medium density field for hydrodynamic simulations,"pyFC" (http://www.ccs.tsukuba.ac.jp/Astro/Members/ayw/code/pyFC/index.html).

-55-