Kitt PeakCorrelation between galaxy and IGM at z=2.2
based on MAMMOTH overdensities mapped by HSC

Yongming Liang
NAOJ / SOKENDAI, M2

Collaborators:
N. Kashikawa, Z. Cai, X. Fan, J. X. Prochaska, K. Shimasaku, M. Tanaka,
H. Uchiyama, R. Shimakawa, M. Onoue, J. Toshikawa, K. Ito.
(Galaxy Evolution Workshop@Kavli IPMU, 2019/06/07)

Structure formation & Evolution:
Cases in Galaxy and Gas?

(CfCP, U. Chicago)

Structure formation & Evolution:
Cases in Galaxy and Gas?

Cosmic Noon
Z~2

Wide Subaru/HSC FOV

Overdensity Tracers
at a certain redshift:

Lyman-Alpha Emitters (LAEs)

g-band

NB387

LMC

D ~ 1.5 deg

(Chiang+2017)

The HSC Field of View (FoV)

Search for Overdensities=
Look for a pin in the ocean ?

MAMMOTH project:
Basic idea
LAEs
(Cai+2016, 2017a)

Lya Forest Sample: SDSS-III/BOSS•Resolution:~ 2000 from 3,600 Å - 10,400 Å~1 Gpc3 @z=2

•Volume:160,000 quasars over 10,000 deg2

•Density:

15 cMpc~20 in one HSC FoV at z=2.5
Image credit: Jeremy Tinker and the SDSS-III collaboration

redshift

15Mpc/h⌧e↵<latexit sha1_base64="HAr7j4d4l5dj79dExNs3RsqULOk=">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</latexit>> 4.5 h⌧e↵ i

Background
QSO

CoSLAsCandidate fields

Subaru/HSC observations
Candidate Fields

Line-of-sights (LoSs)
of background QSOs

Groups of overlapped
Lya absorption (CoSLAs)
g-band: 4 shots x 10 min , ~40 min in total

S17B Queue (30%, 2 fields)
S18B Queue (0%)
S19A On-site (2 fields)…

LAE Selection

NB387: 12 shots x 15 min,~3 hrs in total

Data processing
1. Data reduction is mainly performed with HSC Pipeline v5 & v6.
2. Photometric catalog is obtained from SExtractor.
* Zero-point: Pan-STARS DR1 photometry data

1. Expected NB_HSC from filter transmission for Pickle Stars w. Spectra
2. NB w/ PS1 g, r for fitting curve: NB-g = A + B x (g-r) + C (g-r) 2* PSF matching before the

May cause systematic color bias
# The good quality image (normally
HSC-g image) convolves a Gaussian
kernel to get smoothed to match thatof the other image.

HSC-g

NB387

Photometric Catalog
SExtractor configutations:(1) Dual-image mode with NB387 image as detection image.
(2) Background r.m.s. as weight map to minimize the eﬀect from photometric fluctuation.
(3) The weight maps also work as flag to exclude masked regions (low S/N, saturations, etc.)* MAG_APER for color: d=10 pix (1.7”) except for J0210 with d=15 pix (2.5”)
LAE selection
Selection criteria:
8><g NB387 > 0.83 + h , EW0 > 20Å,
NB387 < mNB.5>:
g NB387 > 3 color + h

LAE candidates<latexit sha1_base64="eUJoEhh9VZLpC4k9gUGLFYkF70M=">AAACynicbVFNi9swEJXdr3X6ld0eexkaWgptjZO0bA6lbFNKe1iWLTSbhSgYWVYcsZJsJHm3wfjWX9hbj/0nlR1Dux8Dgse8eTNvRkkhuLFR9Nvzb92+c/feTtC7/+Dho8f93b0Tk5eashnNRa5PE2KY4IrNLLeCnRaaEZkINk/OPjX8/Jxpw3P13W4KtpQkU3zFKbEuFff/YMFWFnDVC3DCMq4qInimWFr3guAFZPAGsGU/bHU0HU/2a/gAUTgZwytYAz50Ss2ztSVa5xfweR5Hjh9FgCWxa81VVn2sXwPGbatLbd6DjCusJRxNQ3iHDc8kgdpVQhc3jh7DttJJW6Jdv64bN40wwEyl//zj1lsY9wdRGLUB18GwAwPUxXHc/4XTnJaSKUsFMWYxjAq7rIi2nArm+paGFYSekYwtHFREMrPsvMBzl0lhlWv3lIU2+7+iItKYjUxcZXMkc5Vrkjdxi9KuJsuKq6K0TNHtoFUpwObQ/CukXDNqxcYBQjV3XoGuiSbUut/vuSMMr658HZyMwuE4HH17OziYdufYQU/RM/QSDdE+OkBf0TGaIep98aR37l34h772N361LfW9TvMEXQr/518qUdIc</latexit>

LAE candidate sample summary

for color-term correction (h)(Catalog version: 201905c)
g-NB

Latest Results
Ni
1. Revised Overdensity Map: J0210, J0222 (Overdensity: =
N

1,)Ni

<latexit sha1_base64="Fj14whGpzYBLqcAeMy7G8NIQq0A=">AAACE3icbVDNS8MwHE3n15xfVY9egkMQ0dGKoBdh6MXTmOA+YC0lTdMtLG1Kkgqj9H/w4r/ixYMiXr14878x3XrQ6YPA473fS/J7fsKoVJb1ZVQWFpeWV6qrtbX1jc0tc3unK3kqMOlgzrjo+0gSRmPSUVQx0k8EQZHPSM8fXxd+754ISXl8pyYJcSM0jGlIMVJa8swjJyBMIXgJnVAgnLU8mmcO15HixqyV5/AE2sdQ655ZtxrWFPAvsUtSByXanvnpBBynEYkVZkjKgW0lys2QUBQzktecVJIE4TEakoGmMYqIdLPpTjk80EoAQy70iRWcqj8TGYqknES+noyQGsl5rxD/8wapCi/cjMZJqkiMZw+FKYOKw6IgGFBBsGITTRAWVP8V4hHS3ShdY02XYM+v/Jd0Txu21bBvz+rNq7KOKtgD++AQ2OAcNMENaIMOwOABPIEX8Go8Gs/Gm/E+G60YZWYX/ILx8Q1v0J02</latexit>

Eg. Aperture forcounting LAEs

Methods to evaluate overdensity:1). Fixed aperture (Toshikawa+2016) √2). Nearest neighbor distance (Cooper+2005):- 5th nearest neighbor distance ⌃5th = 52⇡r5th3). Gaussian kernel smoothing (Shi+2019)<latexit sha1_base64="vWZqoU3G0qCVMnS0YR9wFJ5SD/4=">AAACF3icbVDLSsNAFJ34rPUVdelmsAiuQlItuhGKblxWtA9oYphMJ+3QmSTMTIQS8hdu/BU3LhRxqzv/xmkbUFsPXDiccy/33hMkjEpl21/GwuLS8spqaa28vrG5tW3u7LZknApMmjhmsegESBJGI9JUVDHSSQRBPGCkHQwvx377nghJ4+hWjRLicdSPaEgxUlryTcu9oX2O/MwVHNbUIIfn0A0Fwlktz9yEQnFX/TFz36zYlj0BnCdOQSqgQMM3P91ejFNOIoUZkrLr2InyMiQUxYzkZTeVJEF4iPqkq2mEOJFeNvkrh4da6cEwFroiBSfq74kMcSlHPNCdHKmBnPXG4n9eN1XhmZfRKEkVifB0UZgyqGI4Dgn2qCBYsZEmCAuqb4V4gHQqSkdZ1iE4sy/Pk1bVco6t6vVJpX5RxFEC++AAHAEHnII6uAIN0AQYPIAn8AJejUfj2Xgz3qetC0Yxswf+wPj4BhJynz8=</latexit>

Aperture size: 5 cMpc
- The typical size for
proto-cluster@z~2.2(Chiang+2013)

Latest Results
1. Overdensity Map: J0924, J1419*Notes for the maps:
1. Considering the large HSC FoV, the mean number density are calculated from each field respectively,
with apertures masked over 10% discarded.
2. For J0222, J0924, J1419, the mean number of LAEs in one aperture is all 4.0, while this number is 2.9.
3. Typically, e.g. for J0924, overdensity of 1.8 (2.4) corresponds to significance of 3.5 (5.7) sigma.

Latest Results
2. OD^2 relation (Optical Depth vs. Over-Density)

15Mpc/hCalculate the ⌧e↵at the corresponding
redshift range from (e)BOSS spectra<latexit sha1_base64="xs0zmhWzfxvr7bxIEHmdlJXtTf8=">AAACEHicbVC7TsMwFHV4lvIKMLJEVAimkiAQjJVYWEBFog+pLZHj3rRWnYfsG0QV5RNY+BUWBhBiZWTjb3DbDNByJFvH59yr63u8WHCFtv1tzM0vLC4tF1aKq2vrG5vm1nZdRYlkUGORiGTTowoED6GGHAU0Ywk08AQ0vMHFyG/cg1Q8Cm9xGEMnoL2Q+5xR1JJrHrQ9P20jTVx9wwOm4PtZdpc6p5PnVcyO+lmWuWbJLttjWLPEyUmJ5Ki65le7G7EkgBCZoEq1HDvGTkolciYgK7YTBTFlA9qDlqYhDUB10vFCmbWvla7lR1KfEK2x+rsjpYFSw8DTlQHFvpr2RuJ/XitB/7yT8jBOEEI2GeQnwsLIGqVjdbkEhmKoCWWS679arE8lZagzLOoQnOmVZ0n9uOzYZefmpFS5zuMokF2yRw6JQ85IhVySKqkRRh7JM3klb8aT8WK8Gx+T0jkj79khf2B8/gCFl54s</latexit>

makecomparison

15cMpcat the⌧e↵ corresponding
LAE &Calculate theposition from our HSC LAEs catalog.
<latexit sha1_base64="0lsgwp6+/OL/ZyIFWMWvWlnbGQY=">AAACI3icbVDLSsNAFJ34rPVVdelmsCiuSiKI4koRoQuFCrYVmhgm05s6OHkwcyOUkH9x46+4caEUNy78F6ePhVoPXDiccy8z5wSpFBpt+9OamZ2bX1gsLZWXV1bX1isbmy2dZIpDkycyUbcB0yBFDE0UKOE2VcCiQEI7eDgf+u1HUFok8Q32U/Ai1otFKDhDI/mVEzdieB+EudsFiczPXRXRy7OLwqXunhlk2ViDMCzuRsw55FcpLwq/UrVr9gh0mjgTUiUTNPzKwO0mPIsgRi6Z1h3HTtHLmULBJRRlN9OQMv7AetAxNGYRaC8fZSzorlG6NEyUmRjpSP15kbNI634UmM1hIv3XG4r/eZ0Mw2MvF3GaIcR8/FCYSYoJHRZGu0IBR9k3hHElzF8pv2eKcTS1lk0Jzt/I06R1UHPsmnPtVE/rkzpKZJvskH3ikCNySuqkQZqEkyfyQt7Iu/VsvVoD62O8OmNNbrbIL1hf36K9pD8=</latexit>
sha1_base64="5Ij7Kl2S7RAhsZ4LfqFfqZBdAsk=">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</latexit>
sha1_base64="jMMT6MWtoYXj1+6eI7rDTLkJMo8=">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</latexit>* BALs and Strong DLAs are carefully checked and excluded.

Latest Results
2. OD^2 relation (Optical Depth vs. Over-Density)

The number of LoS: 33

Previous 2 fields obtained from S17B
A tentative positive correlation ?

Latest Results
2. OD^2 relation (Optical Depth vs. Over-Density)

The number of LoS: 32

Latest 2 fields obtained from S19A

Latest Results
2. OD^2 relation (Optical Depth vs. Over-Density)

Total sample size: 33 -> 65
From the Spearman Test: Correlation: ⇢ = 0.35 with P-value = 0.4%
<latexit sha1_base64="J3u4NDrZfjo2RygthD7HNnYsYgw=">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</latexit>

Latest Results
2. TF-OD relation (Optical Depth translated into Transmission Fluctuation)(Note: Tracer & Scale are somehow diﬀerent)(Mukae+2016)- LAEs@z=2.2- Photo-z galaxies@z=2-3- dz=0.04 (~20pMpc)- dz=25pMpc- 4 MAMMOTH fields covering 5.39 deg2 - COSMOS/Ultra VISTA covering 1.62 deg2
<latexit sha1_base64="F8S5KTwhLokDXfbGp7O1IMS6KBA=">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</latexit>

hF i =

0.26+0.03
0.06

0.079+0.007
0.006 ⇥ gal

3. Cross-Correlation function (Relative)
Estimator:<latexit sha1_base64="36PiXiJbblwZIv6FxLilaKnBfVI=">AAACNHicbZDLSgMxFIYzXmu9VV26CRZBEMtMEXQjFHUh6KJWe4FOKZk004ZmLiQZtQzzUG58EDciuFDErc/gmbYLbT0hycd/ziE5vxMKrrRpvhozs3PzC4uZpezyyuraem5js6aCSFJWpYEIZMMhignus6rmWrBGKBnxHMHqTv8szdfvmFQ88G/1IGQtj3R97nJKNEjt3KV9zzusRzSOsf3AcYLbKXlE96QHdHUDUoJPsO1KQkE4h3WAi3BW8D7sCmTj0d3O5c2COQw8DdYY8mgc5Xbu2e4ENPKYr6kgSjUtM9StmEjNqWBJ1o4UCwntky5rAvrEY6oVD4dO8C4oHewGErav8VD93RETT6mB50BlOo2azKXif7lmpN3jVsz9MNLMp6OH3EhgHeDUQdzhklEtBgCESg5/xbRHwB0NPmfBBGty5GmoFQsW8PVhvnQ6tiODttEO2kMWOkIldIHKqIooekQv6B19GE/Gm/FpfI1KZ4xxzxb6E8b3D9g5pVg=</latexit>

DD⇠bLS =

2DR + RR
Errors are estimated from Jackknife resampling,
RR
which could take the field variance also into account(Landy & Szalay,1993)

LoS location itself has no meaning- But a small sample size may involve
the LoS ‘correlation’ signal?

# From the graph:
1) A statistically significant signal detected at a scale of 0.2 - 3 pMpc (@z=2.2):
a. High optical depth LoSs (HI-rich) correlate with galaxies.
b. Low optical depth LoSs (HI-poor) anti-relate with galaxies.
2) If there is any meaning for the power law fitting parameters here, thecharacteristic scale will be more than 1-order of magnitude smaller thannormal halo CCF?

* UA 2-m Bok observation for fainter background candidates
u-drop sources (Background candidates at z~3)
(B. Cook Lec. Slides, 2013)

No many LoSs in the most
overdense regions?

(Bovy+2011)

Surveys oﬀering deep
g-band (g<24), r-band(r<23.4):• SCUSS, BASS (Zou +2017)

Deep u-band imaging obs using 2-m Bok
Multi-object spectroscopical obs on
MMT/Binospec in the future

20% random sampling withz>2.5 SDSS DR7 quasars

Summary- Deep NB387 imaging with Subaru/HSC to pick out LAEs in the candidate fields with massive
overdensity traced by groups of strong Lya absorption (CoSLAs) in MAMMOTH.

- Built up galaxy overdensity sample.
- Massive large scale structures are mapped.
- Such structures are well traced by CoSLAs
15cMpc15Mpc/h at the position of LoSs.
& ⌧e↵- Compared the LAE and⌧e↵- A global positive correlation hint is found .
- Now the sample size have arise from 33 to 65 due to S19A fields!
- Cross-correlation analysis between galaxy & LoS with High/Low ⌧e↵15Mpc/h .
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15Mpc/h- Higher ⌧e↵
LoSs tends to clustering around galaxies, while the lower one is
opposite at up to 3 pMpc scale -> The constraints on structure formation?
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In the future, maybe we can…
HSC/NB387、NB400
MAMMOTH Overdensities+

Subaru/PFS(Lee+2015)