HI AND METAL ABSORPTION LINES DURING THE EPOCH OF REIONIZATION LUZ - - PowerPoint PPT Presentation

HI AND METAL ABSORPTION LINES DURING THE EPOCH OF REIONIZATION

LUZ ÁNGELA GARCÍA PEÑALOZA ASTRO COLLOQUIUM UNI MELBOURNE, OCTOBER 4TH, 2017

INTRODUCTION

IMPRINTS ON SPECTRA OF HIGH REDSHIFT QUASARS

GP troughs at high z in QSOs spectra

Metal absorption lines

Robertson et al. 2010 Becker et al. 2015

INTRODUCTION

IMPRINTS ON SPECTRA OF HIGH REDSHIFT QUASARS

Credit: Andrew Pontzen

INTRODUCTION

IONIZATION STATES

Low ionization High ionization

e.g. CII, SiII, OI, etc. e.g. CIV, SiIV, OVI, etc. Ionization potential energy ~ H Much larger ionization potential energy than H Expectation to find them in the CGM and regions nearby galaxies. They are detected in the IGM and shock heated gas.

CGM IGM

INTRODUCTION

COLUMN DENSITY & ABSORPTION PATH L

Number of atoms / cm^2 Total survey path length.

INTRODUCTION

SOME STATISTICS: COLUMN DENSITY DISTRIBUTION FUNCTION

What is the distribution of the column density values for a given system ?

INTRODUCTION

SOME STATISTICS: COLUMN DENSITY DISTRIBUTION FUNCTION

What is the distribution of the column density values for a given system ?

F R E Q U E N C Y

Frequency of absorbers per column density bin.

Adapted from Max Pettini’s lectures

INTRODUCTION

SOME STATISTICS: COLUMN DENSITY DISTRIBUTION FUNCTION

What is the distribution of the column density values for a given system ?

F R E Q U E N C Y

First approximation: a single power law !

Adapted from Max Pettini’s lectures

INTRODUCTION

METAL ABSORPTION LINES

Some of these transitions occur redward of Lyα emission (1215 Å). There are many different absorptions the likelihood to be observed increases. The ionic ratios can give us additional information on the conditions of the gas independent from HI. An alternative proxy to study the ionization state of the IGM at high z.

INTRODUCTION

METAL ABSORPTION LINES - CIV

D’Odorico et al. 2013 Díaz et al. in prep.

INTRODUCTION

METAL ABSORPTION LINES - CII

Becker et al. 2011 Finlator et al. 2016

FREQUENCY OF ABSORBERS PER COLUMN DENSITY

INTRODUCTION

NUMERICAL APPROACH:

* INCREASES THE SAMPLE OF ABSORBERS. * TRACES DIFFERENT PHASES OF THE GAS. * REACHES REDSHIFT THAT ARE NOT DETECTED YET WITH OBSERVATIONS. * SPATIAL DISTRIBUTION OF THE ABSORBERS WITH RESPECT TO OTHER OBJECTS.

INTRODUCTION

NUMERICAL APPROACH:

• 1. RUN HIGH-RESOLUTION SIMS

P-GADGET3 (XXL) that includes self-consistent star formation and metal enrichment.

Flat Λ-CDM model is assumed with cosmological parameters from Planck 2015. MDW / EDW: momentum / energy driven winds.

INTRODUCTION

NUMERICAL APPROACH:

• 1. RUN HIGH-RESOLUTION SIMS

Initial conditions at z = 125 Feedback prescriptions Metal enrichment Molecular cooling

INTRODUCTION

NUMERICAL APPROACH:

• 2. ASSUME A UV BACKGROUND CONSISTENT AT HIGH REDSHIFT

Uniform UV ionizing field: radiation background due to the CMB + ultraviolet/X-ray photons from quasars and galaxies with saw-tooth attenuation (Haardt & Madau 2012).

10−4 10−3 10−2 10−1 100 101 102 103 104 105 106 107

E (Ryd)

−35 −30 −25 −20 −15

log Jν (erg/s/cm2/Hz/sr)

z = 8 z = 6 z = 4

INTRODUCTION

NUMERICAL APPROACH:

• 2. ASSUME A UV BACKGROUND CONSISTENT AT HIGH REDSHIFT

Uniform UV ionizing field: radiation background due to the CMB + ultraviolet/X-ray photons from quasars and galaxies with saw-tooth attenuation (Haardt & Madau 2012). Grand sum of ionizing flux from quasars and galaxies

INTRODUCTION

NUMERICAL APPROACH:

• 3. METAL IONS COMPUTED WITH CLOUDY PHOTO-IONIZATION CODE V8.1 FOR

OPTICALLY THIN GAS IN IONIZATION EQUILIBRIUM (FERLAND 2013).

INTRODUCTION

NUMERICAL APPROACH:

• 4. IMPLEMENT A PRESCRIPTION HI SELF-SHIELDING TO ACCURATELY

DESCRIBE THE REGIONS INSIDE THE MASSIVE DARK MATTER HALOS (RAHMATI ET AL. 2013)

INTRODUCTION

NUMERICAL APPROACH:

• 5. GENERATE 1000 RANDOM LINES OF SIGHT INSIDE THE BOX.

INTRODUCTION

NUMERICAL APPROACH:

• 5. GENERATE 1000 RANDOM LINES

OF SIGHT INSIDE THE BOX.

INTRODUCTION

NUMERICAL APPROACH:

• 6. RECOVER THE SPECTRA OF EACH ION IN EACH LINE OF SIGHT

(C II, C IV, SI II, SI IV, O I).

INTRODUCTION

NUMERICAL APPROACH:

• 7. CONVOLVE SYNTHETIC SPECTRA WITH GAUSSIAN NOISE.

INTRODUCTION

NUMERICAL APPROACH:

• 8. USE VOIGT PROFILES TO FIT THE ABSORPTION FEATURES AUTOMATICALLY

WITH THE CODE VPFIT 10.2.

INTRODUCTION

NUMERICAL APPROACH:

• 8. USE VOIGT PROFILES TO FIT THE ABSORPTION FEATURES AUTOMATICALLY

WITH THE CODE VPFIT 10.2.

RESULTS

STAR FORMATION RATE DENSITY

Madau et al. 2014

0.8 dex

RESULTS

STAR FORMATION RATE DENSITY

Madau et al. 2014

4 5 6 7 8

z

4 3 2 1

log SFRD (M yr1 Mpc3)

Absolute magnitude MUV = -17 limit

• Obs. Bouwens+ 2015
• Obs. Bouwens+ 2015 (dust corr)
• Obs. Cucciati+ 2012
• Obs. Hildebrandt and Erben 2010
• Obs. Bouwens+ 2009
• Obs. Ouchi+ 2004
• Obs. Steidel+ 1999

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

García et al. 2017a

RESULTS

CHEMICAL ENRICHMENT

Díaz et al. in prep

0.8 dex Mean metallicity of the Universe: y: amount of heavy metals model SFR IMF stellar yields

RESULTS

4 5 6 7 8

z

10−7 10−6 10−5 10−4

ΩSi

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol 4 5 6 7 8

z

102 103 104

ΩC (10−9)

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

CHEMICAL ENRICHMENT

* Difference between EDW / MDW feedback models. * Consistent with observational constraints at high z.

IGM AND MULTIPHASE GAS

MULTIPHASE GAS

Voids IGM CGM

Star-forming region Shock heated gas

IGM AND MULTIPHASE GAS

MULTIPHASE GAS - METALLICITY

RESULTS

CIV - CDDF CALIBRATION

12.5 13.0 13.5 14.0 14.5 15.0

log NCIV (cm−2)

−19 −18 −17 −16 −15 −14 −13 −12 −11

log fCIV

Obs D’Odorico 5.3 < z < 6.2 f(N)= BN −a f(N)= f(No)(N/No)−a Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

Finlator et al. 2016 García et al. 2017a

Z ~ 5.6

In most works, strong CIV absorbers are quite rare!

RESULTS

CIV - CDDF AT Z ~ 6.4

12.5 13.0 13.5 14.0 14.5 15.0

log NCIV (cm−2)

−17 −16 −15 −14 −13 −12 −11

log fCIV

Obs Bosman+ 17, 6.2 < z < 7.0 Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

RESULTS

CIV COSMOLOGICAL MASS DENSITY

4.0 4.5 5.0 5.5 6.0 6.5 7.0 7.5 8.0

z

10−1 100 101 102

ΩCIV(10−9)

• Obs. Codoreanu+ in prep.
• Obs. Diaz+ in prep.
• Obs. Ryan-Weber+ 09, Pettini+ 03
• Obs. Bosman+ 17
• Obs. D’Odorico+ 13
• Obs. Simcoe+ 11
• Obs. Boksenberg and Sargent 15
• Obs. Songaila 01,05

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

Adapted from García et al. 2017a with new data

RESULTS

C STATES COSMOLOGICAL MASS DENSITY

4.0 4.5 5.0 5.5 6.0 6.5 7.0 7.5 8.0

z

10−1 100 101 102 103

Ω(10−9)

Ch 18 512 MDW

Limits CII Becker+ 06

• Obs. CIV Diaz+ in prep.

CII CIII CIV

Finlator et al. 2015

RESULTS

LAE - CIV absorption pair

Díaz et al. 2015

MUV = -20.7 (detected LAE) LAE: Lyman alpha emitter 212 pkpc = 1360 ckpc LAE wind IGM / CGM metals

RESULTS

LAE - CIV absorption pair

García et al. 2017b

In our simulations, the enrichment of the region cannot be caused by LAEs at a distance of ~1360 ckpc/h at z = 5.6

RESULTS

LAE - CIV absorption pair

García et al. 2017b 500 1000 1500 2000 2500

vel (km/s)

0.0 0.2 0.4 0.6 0.8 1.0

flux CIV A

2000 4000 6000 8000 10000 12000 14000 16000 18000

z (ckpc/h)

−2000 −1000 1000

x (ckpc/h) C

−200 200 400

y (ckpc/h) B

−1000 1000

x (ckpc/h)

−500 500

y (ckpc/h)

CIV abs LAE

Dwarf galaxy d

~ 119 ckpc/h ~ 1296 ckpc/h log NCIV (cm-2)= 14.31

Enrichment is caused by undetected galaxies in the field… the same type of galaxies that complete the budget of ionising photons in the EoR.

RESULTS

LAE - CIV absorption pair

García et al. 2017b

−1000 1000

x (ckpc/h)

−500 500

y (ckpc/h)

CIV abs LAE

Dwarf galaxy d

~ 119 ckpc/h ~ 1296 ckpc/h

Detections with HST proved that there is an undetected galaxy with SFR = 2 Mo / yr in the field, consistent with our prediction for a dwarf galaxy!!

~ 283 ckpc/h

Cai et al. 2017

RESULTS

HI cosmological mass density

García et al. 2017a Neutral pockets of H Tescari et al. 2009

3.5 4.0 4.5 5.0 5.5 6.0

z

1 2 3 4 5

ΩHI (103)

• Obs. Crighton+ 15
• Obs. Prochaska+ 05,09
• Obs. Zafar+ 13

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

RESULTS

HI cosmological mass density

García et al. 2017a Neutral pockets of H Tescari et al. 2009

3.5 4.0 4.5 5.0 5.5 6.0

z

1 2 3 4 5

ΩHI, ΩDLA (10−3)

• Obs. ΩDLA (Bird+ 2017)

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW Ch 18 512 EDW mol Ch 12 512 MDW mol Ch 25 512 MDW mol

• Obs. published after
• ur models predictions

RESULTS

SiIV statistics

Codoreanu et al. in prep.

RESULTS

SiIV cosmological mass density

Codoreanu et al. in prep.

Z ~ 5.6

RESULTS

Conclusions

By using hydrodynamical simulations it is possible to study metal absorption systems that are undetectable with the current observational techniques:

* The evolution of the ionization states of C, in particular CIV are compatible with all of the observations. * The ratio of the comoving mass densities of CII and CIV at z > 6 is raising indicating that the Universe is more neutral at

early times.

* We reproduce the observations of HI at z = 4, especially when molecular cooling is introduced, and make a prediction of

HI content at higher redshift.

* The confirmation of the pair LAE-CIV absorber provides an explanation of the chemical enrichment with metals by

dwarf galaxies.

* Our models reproduce Si IV observed systems and predict high column density absorbers that could be detected in the

future… Stay tuned to Codoreanu et al. in prep.!

IGM AND MULTIPHASE GAS

MULTIPHASE GAS - METALLICITY

RESULTS

Variations of the assumed UVB

10−4 10−3 10−2 10−1 100 101 102 103 104 105 106 107

E (Ryd)

−35 −30 −25 −20 −15

log Jν (erg/s/cm2/Hz/sr)

z = 8 z = 6 z = 4

102 103

λ(˚ A)

−35 −30 −25 −20 −15

log Jν (erg/s/cm2/Hz/sr)

z = 8 z = 6 z = 4

10−4 10−3 10−2 10−1 100 101 102 103 104 105 106 107

E (Ryd)

−35 −30 −25 −20 −15

log Jν (erg/s/cm2/Hz/sr)

z = 6.0 HM12 uni log Jν - 1

García et al. in prep.

RESULTS

Variations of the assumed UVB

10−4 10−3 10−2 10−1 100 101 102 103 104 105 106 107

E (Ryd)

−35 −30 −25 −20 −15

log Jν (erg/s/cm2/Hz/sr)

z = 6.0 HM12 uni log Jν - 1

García et al. in prep.

4.0 4.5 5.0 5.5 6.0 6.5 7.0 7.5 8.0

z

10−1 100 101 102

ΩCIV(10−9)

HM12 uni

• Obs. Diaz+ in prep.
• Obs. Ryan-Weber+ 09, Pettini+ 03
• Obs. Bosman+ 17
• Obs. D’Odorico+ 13
• Obs. Simcoe+ 11
• Obs. Boksenberg and Sargent 15
• Obs. Songaila 01,05

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW

4.0 4.5 5.0 5.5 6.0 6.5 7.0 7.5 8.0

z

10−1 100 101 102

log Jν - 1

Ch 18 512 MDW Ch 18 512 MDW mol Ch 18 512 EDW

Work in progress

RESULTS

Variations of the assumed UVB - II

García et al. in prep.

10−4 10−3 10−2 10−1 100 101 102 103 104 105 106 107

E (Ryd)

−35 −30 −25 −20 −15

log Jν (erg/s/cm2/Hz/sr)

z = 6.0 HM12 uni qua test

RESULTS

DISTRIBUTION OF CII ABSORBERS

13 14 15 16 17 18

log NCII

13 14 15 16 17 18

log NCIV

• Obs. D’Odorico+ 13 z ∼ 6

Random LOV d = 500 ckpc/h d = 100 ckpc/h d = 20 ckpc/h 5 10 15 20 25 30 35 40

Number

5 10 15 20

Number

García et al. 2017a

RESULTS

DISTRIBUTION OF CII ABSORBERS

García et al. in prep.

13 14 15 16 17 0.0 0.1 0.2 0.3 0.4 0.5 0.6

n/ntot

• Obs. Becker+ 06, 5.84 < z < 6.25

Ch 18 512 MDW z = 6

CII

HM12 (original) A B C

RESULTS

LAE - CIV absorption pair

García et al. 2017b

500 1000 1500 2000

d (ckpc/h)

5 10 15 20 25 30

Number All systems 13 < log N < 14 14 < log N < 15 log N > 15

200 400 600 800 1000 1200 1400 1600

d (ckpc/h)

2 4 6 8 10 12 14

Number

LAE Dwarf galaxy

All galaxies Mh > 1.48 x 1010M 1.48 x 109M < Mh < 1.48 x 1010M