1 / 17

Yuichi Matsuda (Tohoku Univ. / NAO Japan) collaborators Toru Yamada (NAO Japan)

Lyman alpha blobs in a Large-Scale Structure at z=3.1. Yuichi Matsuda (Tohoku Univ. / NAO Japan) collaborators Toru Yamada (NAO Japan) Tomoki Hayashino (Tohoku Univ.) et al. Y. Matsuda et al., AJ, 2004, in press

kael
Télécharger la présentation

Yuichi Matsuda (Tohoku Univ. / NAO Japan) collaborators Toru Yamada (NAO Japan)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Lyman alpha blobs in a Large-Scale Structure at z=3.1 Yuichi Matsuda (Tohoku Univ. / NAO Japan) collaborators Toru Yamada (NAO Japan) Tomoki Hayashino (Tohoku Univ.) et al. Y. Matsuda et al., AJ, 2004, in press T. Hayashino et al., AJ, 2004, in press

  2. Outline The protocluster at z=3.1 in SSA22 is one of the best field to study high-z galaxies in high density region The previous survey (9’ x 9’) 70 Lyman alpha emitters (Steidel et al. 2000) 2 Lyman alpha blobs Our NB survey (32’ x 24’) 283 Lyman alpha emitters (Hayashino et al. 2004) 35 Lyman alpha blobs (1) A belt-like structure of Lyman alpha emitters (length ≥60 Mpc in comoving scale) (2) The first large sample of Lyman alpha blobs (size = 30-200 kpc in physical scale)

  3. Our target field The protoclusterat z=3.1 in SSA22 (Steidel et al. 1998, 2000) Redshift distribution of Lyman-break galaxies z=3.1 peak The SSA22 z=3.1 peak of Lyman-break galaxies has δρgal/ρgal = 5 in 16 x 16 x 37 Mpc N The SSA22 z=3.1 peak is the largest peak in their 17 survey fields of Lyman-break galaxies at z~3 Redshift

  4. Our target field The protoclusterat z=3.1 in SSA22 (Steidel et al. 1998, 2000) Steidel et al. (2000) got a deep narrow-band image of the protocluster. 16Mpc They found 70 Lyman alpha emitters. 16Mpc

  5. Our target field The protoclusterat z=3.1 in SSA22 (Steidel et al. 1998, 2000) They also found 2 giant (~200kpc) Lyman alpha blobs. 300kpc Blob1 and Blob2 have Sub-mm sources. (Chapman et al. 2001) SFR ~ 1000 Mo/yr Formation of massive galaxies? Continuum Lyman alpha

  6. Our observation We got 9 times wider and 0.4 mag deeper narrow-band image of the SSA22 protocluster at z=3.1 Our field of view 32’ x 24’ Steidel et al. (2000) 9’ x 9’ Subaru 8m telescope Suprime-Cam Narrow-band filter 7.2 hour exposure!! 45Mpc 60Mpc

  7. (1) Large scale structure at z=3.1 We found a belt-like structure of ~300 Lyman alpha emitters (length ≥ 60 Mpc in comoving scale) Our field of view 32’ x 24’ 283 Lyman alpha emitters Photometry 2” diameter aperture Lyman alpha flux > 2 x 10-17 ergs/s/cm2 EWobs > 170A 45Mpc Lyman alpha blobs δρgal/ρgal ~ 2 60Mpc

  8. (1) Large scale structure at z=3.1 Large filament of emitters (length ≥ 60 Mpc & radius ~10Mpc) 56 spectroscopically confirmed Lyman alpha emitters at z=3.1 Subaru 8m telescope FOCAS MOS 0.8-1.5 hour exposure!! 45Mpc No contamination by [OII] and [OIII] emitters 60Mpc

  9. (2) Lyman alpha blobs We could resolved detail structures 300kpc Green shows Lyman alpha 200 kpc Continuum Lyman alpha Steidel et al. (2000) Our deep images

  10. (2) Lyman alpha blobs We found 33 new Lyman alpha blobs Lyman alpha emitters 35 Lyman alpha blobs Photometry isophotal aperture Lyman alpha flux > 7 x 10-17 ergs/s/cm2 EWobs>80A Size > 30 kpc Lyman alpha blobs are more concentrated!! 45Mpc Blob1 and Blob2 δρgal/ρgal ~2 60Mpc

  11. (2) Lyman alpha blobs 35 Lyman alpha blobs have large varieties Blob1 Blob2 The first large sample of Lyman alpha blobs 200kpc

  12. (2) Lyman alpha blobs Large varieties different origins? (1) Photoionization by massive stars or by AGN (in some cases … may be hidden by dust) (2) Cooling radiation in collapsing halo (e.g. Haiman et al. 2000) (early phase of galaxy formation) (3) Galactic superwind (e.g. Taniguchi & Shioya 2000) (late phase of intense star formation) Plus, scattering..

  13. (2) Lyman alpha blobs Lyman alpha flux vs. UV continuum flux Choice of the continuum object: the nearest source to the Lyman alpha peak, or the known LBG Blob1 Blob2 Lyman alpha Excess 14 / 35 blobs show Lyman alpha Excess to the massive star photoionization (no dust, Salpeter IMF).

  14. (2) Lyman alpha blobs Conical structure Galactic superwind? 200kpc

  15. (2) Lyman alpha blobs Blob1 Bubble-like structure Galactic superwind? (see also Ohyama et al. 2003) or Cooling radiation? Velocity structure is chaotic (Bower et al. 2004) 200kpc

  16. (2) Lyman alpha blobs Cooling radiation from collapsing halo? Diffuse nebulae & No plausible continuum source 200kpc

  17. Summary The protocluster at z=3.1 in SSA22 has (1) Large filament of Lyman alpha emitters (length ≥60 Mpc in comoving scale) (2) 35 Lyman alpha blobs ( size = 30-100 kpc in physical scale) The first large sample of Lyman alpha blobs More concentrated then emitters Blob1 and Blob2 are the largest and the brightest blobs 1/3 has Lyman alpha excess to massive star photoionization Good sample of forming galaxies in high density region at high redshift

More Related