Strategy for Japan-Italy Seminar 2003Strategy for Japan-Italy Seminar 2003

Formation of the First Generation of Galaxies: Strategy for the Observational CorrFormation of the First Generation of Galaxies: Strategy for the Observational Corroboration of Physical Scenariosoboration of Physical Scenarios

第一世代銀河の形成： 物理的シナリオの観測的実証へ向けての戦略第一世代銀河の形成： 物理的シナリオの観測的実証へ向けての戦略

December 1-6, 2003, Niigata University, JAPANDecember 1-6, 2003, Niigata University, JAPAN

ParticipantsParticipantsMembers on Italy SideMembers on Italy Side

Andrea Ferrara (Chair)Andrea Ferrara (Chair)Raffaella SchneiderRaffaella SchneiderMarialuce BruscoliMarialuce BruscoliSimone MarriSimone MarriAntonella Maselli Antonella Maselli Ruben SalvaterraRuben SalvaterraSimone Bianchi Marialuce Bruscoli Benedetta Ciardi Alessio Fangano Francesco Haardt Hiroyuki Hirashita Ilian Iliev Simone Marri Antonella Maselli Vladimiro Noce Phillip Richter Ruben Salvaterra Evan Scannapieco Raffaella Schneider Filippo Sigward Marcos Valdes

Members on Japan SideMembers on Japan Side

梅村雅之梅村雅之 (Chair) (Chair) 中本泰史中本泰史米原厚憲米原厚憲廣居久美子廣居久美子西亮一西亮一水澤広美水澤広美須佐元須佐元森正夫森正夫北山哲北山哲大向一行大向一行

Japan-Italy Seminar 2002Japan-Italy Seminar 2002July 8-10, 2002, Arcetri Obs, Firenze, Italy

Topics coveredTopics covered

1. Formation and evolution of the population III stars, which includes the stellar 1. Formation and evolution of the population III stars, which includes the stellar collapse and the resultant initial mass function. collapse and the resultant initial mass function.

2. Formation of primordial objects with taking into accounts the radiative feedback 2. Formation of primordial objects with taking into accounts the radiative feedback around first luminous objects around first luminous objects

3. Dynamical and chemical feedback by supernovae. 3. Dynamical and chemical feedback by supernovae.

4. Inhomogeneous reionization of the universe based on multi-dimensional radiative 4. Inhomogeneous reionization of the universe based on multi-dimensional radiative transfer calculations. transfer calculations.

5. Formation and evolution of galaxies with focusing on UV background effects and 5. Formation and evolution of galaxies with focusing on UV background effects and supernova effects. supernova effects.

6. Observations of high redshift universe, which include the IR background 6. Observations of high redshift universe, which include the IR background

7. IR emission by high redshift hydrogen molecules and dust 7. IR emission by high redshift hydrogen molecules and dust

8. QSO absorption lines as tools to investigate the IGM 8. QSO absorption lines as tools to investigate the IGM

ProgramProgram Monday June 08th, 2002Monday June 08th, 2002

09:25 A. FERRARA Welcome 09:25 A. FERRARA Welcome

SESSION I : FIRST STARS AND OBSERVABLE EFFECTSSESSION I : FIRST STARS AND OBSERVABLE EFFECTS

09:30 K. OMUKAI Formation of First Stars by Accretion 09:30 K. OMUKAI Formation of First Stars by Accretion 10:00 M. UMEMURA The IMF of Pop III Stars and its Influence on the Growth of First Objects 10:00 M. UMEMURA The IMF of Pop III Stars and its Influence on the Growth of First Objects 10:30 R. NISHI On the Formation Sites and the Mass Scales of Pop III Stars 10:30 R. NISHI On the Formation Sites and the Mass Scales of Pop III Stars 11:30 R. SCHNEIDER First Stars, Black Holes and Particles: Signals from the Dark Ages 11:30 R. SCHNEIDER First Stars, Black Holes and Particles: Signals from the Dark Ages 12:00 R. SALVATERRA First stars and the Near Infrared Background 12:00 R. SALVATERRA First stars and the Near Infrared Background

12:30 ________ Lunch Break __________ 12:30 ________ Lunch Break __________

SESSION II: PRIMORDIAL OBJECTS AND FEEDBACKSSESSION II: PRIMORDIAL OBJECTS AND FEEDBACKS

14:30 F. HAARDT From first stars to reionization (via supermassive black holes) 14:30 F. HAARDT From first stars to reionization (via supermassive black holes) 15:00 B. CIARDI Simulating IGM Reionization: Progresses, Problems and Promises 15:00 B. CIARDI Simulating IGM Reionization: Progresses, Problems and Promises 15:30 T. KITAYAMA Radiative Feedback Effects on Primordial Galaxy Formation 15:30 T. KITAYAMA Radiative Feedback Effects on Primordial Galaxy Formation 16:30 H. SUSA Formation of Subgalactic Objects in the Presence of UV Radiation 16:30 H. SUSA Formation of Subgalactic Objects in the Presence of UV Radiation

Tuesday June 09th, 2002Tuesday June 09th, 2002

SESSION III: GALAXY FORMATION AND EVOLUTIONSESSION III: GALAXY FORMATION AND EVOLUTION

09:30 H. HIRASHITA Effect of Dust Grains on High-Redshift Star Formation History 09:30 H. HIRASHITA Effect of Dust Grains on High-Redshift Star Formation History 10:00 A. YONEHARA Toward Direct Detection of Substructure Around Galaxies 10:00 A. YONEHARA Toward Direct Detection of Substructure Around Galaxies 10:30 M. MORI Inhomogeneous Metal Enrichment by Multiple Supernovae 10:30 M. MORI Inhomogeneous Metal Enrichment by Multiple Supernovae

SESSION IV: REIONIZATION AND RADIATIVE TRANSFERSESSION IV: REIONIZATION AND RADIATIVE TRANSFER 11:30 T. NAKAMOTO Toward a New Accurate Multi-dimensional Radiative Transfer Solver 11:30 T. NAKAMOTO Toward a New Accurate Multi-dimensional Radiative Transfer Solver 12:00 A. MASELLI CRASH: A new Cosmological RAdiative transfer Scheme for Hydrodynamics 12:00 A. MASELLI CRASH: A new Cosmological RAdiative transfer Scheme for Hydrodynamics

12:30 ________ Lunch Break __________ 12:30 ________ Lunch Break __________

14:30 I. ILIEV On the Direct Detectability of the Cosmic Dark Ages: 21-cm Emission from Minihalos 14:30 I. ILIEV On the Direct Detectability of the Cosmic Dark Ages: 21-cm Emission from Minihalos

SESSION V: INTERGALACTIC MEDIUMSESSION V: INTERGALACTIC MEDIUM 15:00 S. MARRI Numerical Simulation of Galaxy Formation and Evolution in LCDM models: Energy Feedback and Metal Enrichment from Star Formation 15:00 S. MARRI Numerical Simulation of Galaxy Formation and Evolution in LCDM models: Energy Feedback and Metal Enrichment from Star Formation 15:30 M. BRUSCOLI Reionization - Background Radiation 15:30 M. BRUSCOLI Reionization - Background Radiation 16:30 S. BIANCHI IGM Metal Enrichment through Dust Sputtering 16:30 S. BIANCHI IGM Metal Enrichment through Dust Sputtering 17:00 P. RICHTER H_2 absorption line measurements in the Local Group 17:00 P. RICHTER H_2 absorption line measurements in the Local Group

Wednesday June 10th, 2002Wednesday June 10th, 2002

SESSION VI: GENERAL DISCUSSIONSESSION VI: GENERAL DISCUSSION

09:30 A. FERRARA Summary & Overview of Collaborative Areas 09:30 A. FERRARA Summary & Overview of Collaborative Areas > A GENERAL DISCUSSION FOLLOWS > A GENERAL DISCUSSION FOLLOWS

PARALLEL GROUP DISCUSSIONSPARALLEL GROUP DISCUSSIONS

10:30 The Seminar will now be split into a few parallel groups based on the 10:30 The Seminar will now be split into a few parallel groups based on the Collaborative Areas individuated in the previous discussion. Participants Collaborative Areas individuated in the previous discussion. Participants can join one of the groups to which they feel they can contribute the most can join one of the groups to which they feel they can contribute the most with the aim of setting up a joint collaboration. One of the members of with the aim of setting up a joint collaboration. One of the members of such groups will report on the results of the discussion and possibly on such groups will report on the results of the discussion and possibly on the general l ines of the research project selected for collaboration. the general l ines of the research project selected for collaboration.

12:30 ________ Lunch Break __________ 12:30 ________ Lunch Break __________

PARALLEL GROUP REPORTSPARALLEL GROUP REPORTS

16:30 The plenary session is resumed and a member of the groups will give 16:30 The plenary session is resumed and a member of the groups will give a ~10 min summary of the discussion a ~10 min summary of the discussion

AREA I. First StarAREA I. First StarChair M. UmemuraChair M. Umemura

AREA II. Galaxy Formation and FeedbackAREA II. Galaxy Formation and FeedbackChair H. SusaChair H. Susa

AREA III. AREA III. Reionization/RadTrans/IGMChair B. CiardiChair B. Ciardi

Parallel Discussion for Future CollaborationsParallel Discussion for Future Collaborations

Possible CollaborationsPossible Collaborations

AREA I. First StarAREA I. First Star

Raffaella, Ruben, Nishi, Omukai, Mizusawa, SaigoRaffaella, Ruben, Nishi, Omukai, Mizusawa, Saigo**, Umemura, Umemura

1. Role of Dark Matter for Fragmentation of Cylindrical Clouds (with Metal) 1. Role of Dark Matter for Fragmentation of Cylindrical Clouds (with Metal) - - Nishi, Omukai, MU, (Saigo)Nishi, Omukai, MU, (Saigo)

DM: 3D N-body, hydrodynamics: 1DDM: 3D N-body, hydrodynamics: 1D

2. Role of Dark Matter for Spherical Runaway in Early Phase of Collapse2. Role of Dark Matter for Spherical Runaway in Early Phase of Collapse - - Nishi, Omukai, Nishi, Omukai, SusaSusa, (Saigo), (Saigo)

3. Inverse Problem of Abundance Ratio to Place Constraints on the IMF 3. Inverse Problem of Abundance Ratio to Place Constraints on the IMF of Pop III Stars - of Pop III Stars - Raffaella, Ruben, MU, (Nakamura)Raffaella, Ruben, MU, (Nakamura)

abundance ratio of ICM, DLA (Si, O, Fe, Zn) = AREA IIIabundance ratio of ICM, DLA (Si, O, Fe, Zn) = AREA IIIconsistency with IR backgroundconsistency with IR background

4. High Mass Limit of Pop III Stars by Accretion 4. High Mass Limit of Pop III Stars by Accretion - - Omukai, Raffaella, MizusawaOmukai, Raffaella, Mizusawa

metallicity dependence, time-dependence (RHD)metallicity dependence, time-dependence (RHD)fragmentationfragmentation

5. Spectrum of Pop III ZAMS with Accreting Envelop - 5. Spectrum of Pop III ZAMS with Accreting Envelop - Omukai, Ruben Omukai, Ruben color, IR background, reionizationcolor, IR background, reionization

6. BH Remnants interacting with Ambient Matter in PopIII Objects6. BH Remnants interacting with Ambient Matter in PopIII Objects - - Nishi, Raffaella, Susa (Saigo)Nishi, Raffaella, Susa (Saigo)

Bondi (Hoyle-Littleton) accretion onto BHsBondi (Hoyle-Littleton) accretion onto BHs radiative feedback for further SFradiative feedback for further SF

7. High-z GRBs - 7. High-z GRBs - Raffaella, MURaffaella, MUall possible observational features all possible observational features

((-burst, X-ray burst, -burst, X-ray burst, -CMB interaction)-CMB interaction)

(8.) VMBHs(8.) VMBHsgravitational lensing by intergalactic MBHsgravitational lensing by intergalactic MBHsless massive BH interacting halo starsless massive BH interacting halo stars

Possible CollaborationsPossible Collaborations

AREA II. Galaxy Formation and FeedbackAREA II. Galaxy Formation and Feedback

Hirashita, Kitayama, Mori, Marri, Richter, Sigward, Susa,Yonehara Hirashita, Kitayama, Mori, Marri, Richter, Sigward, Susa,Yonehara

1. On the Reliability of Large-scale Simulation of Metal Ejection - 1. On the Reliability of Large-scale Simulation of Metal Ejection - Mori, MarriMori, Marri

Two phase treatment of MSPH feedbackTwo phase treatment of MSPH feedback

Adjust the parameter of MSPH by high resolution simulations.Adjust the parameter of MSPH by high resolution simulations.

2. GF Simulations with Dust and its Observational Possibilities 2. GF Simulations with Dust and its Observational Possibilities

Hirashita, Mori,…Hirashita, Mori,…

GF(SN) simulations + dust → how it looks like?GF(SN) simulations + dust → how it looks like?

Hirashita, Susa,…Hirashita, Susa,…

GF simulations by RSPH + dust (low metal)GF simulations by RSPH + dust (low metal)

Both of Low mass & High massBoth of Low mass & High mass

3. DLA H2 Phase3. DLA H2 Phase

Hirashita, Mori, Richter, SusaHirashita, Mori, Richter, Susa

Small fraction of H2 in DLASmall fraction of H2 in DLA

→ → small coverage factorsmall coverage factor

Numerical simulation of Forming galaxies with dust (product of numerical siNumerical simulation of Forming galaxies with dust (product of numerical simulations)mulations)

Find the detection probability of high H2 regions Find the detection probability of high H2 regions

4. Observed Dust Distribution in Galaxies and Reddening of QSO 4. Observed Dust Distribution in Galaxies and Reddening of QSO Multiple Images Multiple Images

Richter,YoneharaRichter,Yonehara

Observed distribution of dust in a galaxyObserved distribution of dust in a galaxy

Evaluation of reddening of each imageEvaluation of reddening of each image

→ → Information on QSO microlensing Information on QSO microlensing

This is also for inter group collaborations with Bianchi, Ferrara…This is also for inter group collaborations with Bianchi, Ferrara…

AREA III. Reionization/RadTrans/IGM

Task Leader/Reporter: Task Leader/Reporter: CiardiCiardiSuggested Members: Suggested Members: Bianchi, Bruscoli, Ferrara, Iliev, Maselli, Nakamoto, Hiroi, GalleraniBianchi, Bruscoli, Ferrara, Iliev, Maselli, Nakamoto, Hiroi, Gallerani

Meeting Room: Meeting Room: Aula AAula A

ART ART CRASH CRASH CORAL CORAL

SOURCESOURCE

Point Point MultipleMultiple BackgroundBackground Location any any out of grid Location any any out of grid Spectrum monochromatic any anySpectrum monochromatic any anyEvolution Evolution

H/HeH/He TemperatureTemperature Re-emissionRe-emission Distrib/Dynamic RangeDistrib/Dynamic Range

Hydrodynamics Hydrodynamics Time dependentTime dependent Dimensionality 3DDimensionality 3D 3D 3D 2D2D

GASGAS

ADDITIONAL ADDITIONAL

1. Comparison between different codes for the radiative transfer1. Comparison between different codes for the radiative transfer

Common Test for the Codes

recsim

c

H

tt

eVSpectrum

cornerpositionSource

kpcL

sphotN

N

mequilibriux

cmn

KT

5

6.13:

:

6.6

10

128

10

10

148

3

33

4

RUN I:RUN I:

RUN III: Realistic spectrumRUN III: Realistic spectrum

RUN II: Realistic density fieldRUN II: Realistic density field

DEADLINE:DEADLINE:

October 31st!!!October 31st!!!

Japan-Italy Seminar 2003Japan-Italy Seminar 2003

Formation of the First Generation of Galaxies: Strategy for the Observational CorrFormation of the First Generation of Galaxies: Strategy for the Observational Corroboration of Physical Scenariosoboration of Physical Scenarios

December 1-6, 2003, Niigata University, JAPANDecember 1-6, 2003, Niigata University, JAPAN

ParticipantsParticipants

Members on Italy SideMembers on Italy Side

Andrea Ferrara (Chair)Andrea Ferrara (Chair)Raffaella SchneiderRaffaella SchneiderMarialuce BruscoliMarialuce BruscoliSimone MarriSimone MarriAntonella Maselli Antonella Maselli Ruben SalvaterraRuben Salvaterra

Members on Japan SideMembers on Japan Side

西亮一 西亮一 (Chair)(Chair) ，，中村文隆，中村文隆，水澤広美　（新潟大）水澤広美　（新潟大）梅村雅之，梅村雅之，中本泰史，中本泰史，米原厚憲，米原厚憲，廣居久美子　（筑波大）廣居久美子　（筑波大）須佐元 （立教大）須佐元 （立教大）森正夫 （専修大）森正夫 （専修大）北山哲 （東邦大）北山哲 （東邦大）大向一行，大向一行，西合一矢（国立天文台）西合一矢（国立天文台）平下博之（名大）平下博之（名大）

Invited SpeakersInvited Speakers

野本憲一，野本憲一，梅田秀之，梅田秀之，岩本信之，岩本信之，中里直人（東大）中里直人（東大）吉田直紀，吉田直紀，矢作日出樹（国立天文台）矢作日出樹（国立天文台）松原隆彦（名大）松原隆彦（名大）釣部通（阪大）釣部通（阪大）小笹隆司（北大）小笹隆司（北大）牧秀樹（立教大）牧秀樹（立教大）佐藤潤一，佐藤潤一，川勝望，川勝望，Alex RazoumovAlex Razoumov （筑波大）（筑波大）

OrganizationOrganization

Welcome address: R. NishiWelcome address: R. Nishi

SESSION I. FORMATION AND EVOLUTION OF FIRST STARSSESSION I. FORMATION AND EVOLUTION OF FIRST STARS

SESSION II. FORMATION OF PRIMORDIAL OBJECTSSESSION II. FORMATION OF PRIMORDIAL OBJECTS

SESSION III. INHOMOGENEOUS REIONIZATION AND THERMAL EVOLUTION OF IGMSESSION III. INHOMOGENEOUS REIONIZATION AND THERMAL EVOLUTION OF IGM

SESSION IV. FORMATION AND EVOLUTION OF GALAXIESSESSION IV. FORMATION AND EVOLUTION OF GALAXIES

SESSION V. OBSERVATIONS OF HIGH REDSHIFT UNIVERSESESSION V. OBSERVATIONS OF HIGH REDSHIFT UNIVERSE

SESSION VI. FORMATION AND EVOLUTION OF SMBHs AND AGNsSESSION VI. FORMATION AND EVOLUTION OF SMBHs AND AGNs

SESSION VII: SUMMARY & OVERVIEWSESSION VII: SUMMARY & OVERVIEW

SESSION VIII: PRENARY PANEL DISCUSSIONSESSION VIII: PRENARY PANEL DISCUSSION

----------------------------------------------------------------------------------------------------------------------------------------------------------------

PARALLEL SCIENTIFIC DISCUSSIONSPARALLEL SCIENTIFIC DISCUSSIONS

PARALLEL REPORTSPARALLEL REPORTS

R. Nishi ?R. Nishi ?

Panel Discussion on Numerical Technique Panel Discussion on Numerical Technique

PanelistsPanelists

Baryon Baryon Dark matter(Stars) Dark matter(Stars) Radiation Radiation Enrichment Enrichment Hydrodynamics N-body Radiative Transfer ChemistryHydrodynamics N-body Radiative Transfer Chemistry

Andrea Ferrara Andrea Ferrara Simone MarriSimone Marri中村文隆中村文隆中本泰史中本泰史須佐元須佐元森正夫森正夫西合一矢西合一矢平下博之平下博之中里直人中里直人吉田直紀吉田直紀矢作日出樹矢作日出樹釣部通釣部通小笹隆司小笹隆司佐藤潤一佐藤潤一Alex RazoumovAlex Razoumov

Chair: MU??????Chair: MU??????

AREA I. First StarAREA I. First StarChair ? Chair ?

AREA II. Galaxy Formation and EvolutionAREA II. Galaxy Formation and EvolutionChair ? Chair ?

AREA III. Metal and DustAREA III. Metal and DustChair ? Chair ?

Parallel Scientific DiscussionParallel Scientific Discussion

Parallel ReportsParallel Reports

15min/group15min/group

RaffaellaRaffaella

Mori, Yoshida Mori, Yoshida

AndreaAndrea

日伊セミナー第一世代銀河の形成： 物理的シナリオの観測的実証へ向けての戦略（ Formation of the First Generation of Galaxies: Strategy for the Observational Corroboration of Physical Scenarios ）

科研費基盤（Ｂ）「第一世代天体形成の包括的研究」 H15 － H17

　梅村 雅之，中本 泰史，西合 一矢，西 亮一，中村 文隆，須佐 元

Thank youThank you