Myung Gyoon Lee. Seoul National University (SNU), Korea. The 7 th Survey Science Workshop, Jan 15-17, 2018, High-1 Resort, Korea
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1 Myung Gyoon Lee with In Sung Jang (AIP) Department of Physics & Astronomy Seoul National University (SNU), Korea The 7 th Survey Science Workshop, Jan 15-17, 2018, High-1 Resort, Korea 1
2 H 0 Today s Expansion rate of the Universe 2
3 Two Ways to Estimate H 0 H(t=t 0 ) cosmic distance ladder H(z)->H(t 0 ) inverse distance ladder (CMBR, BAO) 3
4 Cosmic Distance ladder for H 0 SN Ia Cosmology->H(t 0 ) Calibration of SN Ia: Cepheids based on geometric anchors 4
5 The status of H 0 in 2016 Cepheids have been used to calibrate SN Ia. Cepheid-calibrated SN Ia & CMB are diverging in H 0 estimates! 5
6 SN Ia(Cepheids) +Mould, Kennicutt CMB
7 Four possibilities: xo, ox, xx, oo? SN Ia(Cepheids)? CMB
8 By independent calibration of SN Ia using the TRGB! 8
9 Cosmic Distance ladder for H 0 SN Ia Cosmology->H(t 0 ) Calibration of SN Ia: Cepheids based on geometric anchors TRGB based on geometric anchors 9
10 10
11 -The resolution of M32, NGC 205 & the central region of M31. -Resolved stars are similar to those of globular clusters (Pop II). -Mpg (TRGB) = -1.1 mag TRGB Mvis GC MWG (Pop I) Spectral type 1 1
12 The TRGB has become popular as a precise distance indicator, due to following factors. (1) Edge detection and the TRGB precision Lee, Freedman, & Madore (1993) The TRGB as a Distance Indicator for Resolved Galaxies -an edge detector (Sobel filters) for the TRGB measurement, -the precision of the TRGB is comparable to that of Cepheids. -M I (TRGB) = -4.0±0.1 (m-m) 0 (TRGB) (2) Advent of HST (1990-) (m-m) 0 (Cepheid, RR Lyrae) 12
13 Today, the TRGB is a powerful tool for SN cosmology to determine the Hubble Constant! (Beaton+2016, Jang & Lee2017a,b and references therein). 13
14 Leo A (SF Irr) SN Ia are found in all types of galaxies. Galaxies have stars with a large range of ages, including many old stars! (1) The TRGB can be used for any types of resolved galaxies. (2) Suffers little extinction problem. (3) for d<35 Mpc with HST (2017). Leo A (SF Irr) Tolstoy (2009) 14
15 TIPSNU: The Tip of the RGB for SN host galaxies in the Universe at Seoul National University! 15
16 (1) Improving the accuracy and the precision of the TRGB. (2) Increasing the sample of SN Ia for calibration. 16
17 TIPSNU IV. (Jang & Lee 2017a, ApJ, 835, 28) (1) Higher Precision -deriving TRGBs for a large range of color -introducing QT magnitude, which is a colorindependent magnitude of the TRGB. -using the Sobel filter for edge detection. -typical measuring error of the TRGB: ~0.02mag 17
18 -Targets: nearby galaxies of various types (E, Irr, S) with deep HST images -typical measuring error of TRGB: ~1% 18
19
20 TIPSNU IV. (Jang & Lee 2017a) -Derived QT magnitude, which is a colorindependent magnitude of the TRGB: QT= I ((V-I) 0-1.5) ((V-I) 0-1.5) -using blue RGBs -typical measuring error of TRGB: ~0.02mag 20
21 TIPSNU IV. (Jang & Lee 2017a, ApJ) (2) Higher Accuracy -Previous calibrations are based on HBs in MW GCs or Local Group galaxies. -In contrast, TIPSNU uses two distance anchors with geometric distance estimates. -systematic error of the TRGB distance: ~2.7% 21
22 Two distance anchors with accurate geometric distances 1) NGC 4258 (M106, based on H 2 O Megamasers) 2) The LMC (based on 8 eclipsing binaries)
23 M I = -4.05±0.12 (Bellazzini+01) M I = ±0.096 = ±0.073 M I = ±0.058 (Our best estimate) Accurate to 2.7% of distance
24 -Excellent agreement with Lee+(1993) for low metallicity! -Note that they based on totally independent calibrations! TIPSNU (Jang & Lee 2017a) 24
25 -TIPSNU.V. (Jang & Lee2017b, ApJ, 836,74)
26 TIPSNU (The Tip of the RGB for SN host galaxies in the Universe) Criteria for targets -Galaxies at <40 Mpc hosting SN Ia with HST images -with modern photometry of SN Ia -with low extinction In 2017: N(SN Ia)=8 Current Progress: I: M101 (Lee & Jang 2012, ApJL, 760, L14) II: M66 and M96 (Lee & Jang 2013, ApJ, 773, 13) III: NGC 4038/39, NGC 5584 (Jang & Lee 2015, ApJ, 807, 133) IV: New TRGB calibration (Jang & Lee 2017a, ApJ, 835, 28) V: NGC 3021 and others (Jang & Lee 2017b, ApJ, 836, 74) 26
27 Impossible to get TRGB distances? The most challenging sample for TRGB! 27
28 NGC 3370 : SN 1994ae NGC 3021 : SN 1995al F555W : 57,600s F814W : 24,000s (m-m)0,cep = 32.13±0.07 (Riess+11) d~27 Mpc (m-m)0,cep = 32.27±0.08 (Riess+11) d~28 Mpc
29 NGC 1309 : SN 2002fk (The Champion in TRGB) (m-m)0,cep = 32.59±0.09 (Riess+11) d~33 Mpc F555W : 57,600s F814W : 24,000s
30
31 -N (low reddened SN Ia) = 6 -M v (SN Ia) = ±0.06 (ran)±0.06(sys)
32 Riess et al. (2016) Mega-SH0ES A 2.4% determination of the local value of H 0 Cepheid distance estimate: for 19 SN Ia SN Ia in nearby universe (z<0.1) : 233 SNe Ia H 0 = ± 1.74 km/s/mpc (2.4% error) Riess et al. (2009, 2011) SH0ES Cepheid (MW,LMC) and Maser distance estimate : for 8 SN Ia SN Ia in nearby universe (z<0.1) : 140 SNe Ia H 0 = 73.8 ± 2.4 km/s/mpc (4.1% error) 32
33 For the 6 low-reddened SN Ia, We use m B,corr (Riess+16)+ TRGB distances (Jang&Lee17). SN Ia Hubble Diagram for 233 SN Ia (Riess+16) Log(H 0 ) = 0.2M B +a B +5 a B = Weighted Mean of 6 SNe : M B,corr = ±0.07 H 0 = 71.2 ±2.5 (3.5%) (±0.051 r ±0.046 s mag) (±1.66 r ±1.87 s km/s/mpc) Our best estimate!
34 TIPSNU value (Jang & Lee2017b) based on M106 and LMC anchors H 0 = ± 2.50 km/s/mpc (3.5% error) is in excellent agreement with (Riess+2016) s value based on M106 and LMC, H 0 = ±1.78 km/s/mpc, but, is 1.07 km/s/mpc smaller than (Riess+2016) s value based on four anchors (including M31, MW), H 0 = ±1.74 km/s/mpc (2.4% error).
35 Mystery for NGC 4038/39 Why such a large difference in Cepheid distances? NGC 4038/39 : SN 2007sr (Antennae galaxies)
36 Mystery for NGC 4038/39! : SN 2007sr (Antennae galaxies) Cepheid distances Riess+(2011) used the entire Cepheid sample: (m-m) 0 =31.66±0.08 Riess+(2016) excluded 10 ULP Cepheids (P>80d): (m-m) 0 =31.290±0.112 TRGB distance (JL2017) (m-m) 0 =31.677±0.037 is consistent with Riess+(2011) value, but not with Riess+(2016)! A problem for Cepheid distances: Should we include or exclude ULP for Cepheid distance estimates? -Need to be studied in the future!
37 ?
38 SN Ia(Cepheid based on 4 anchors) PLANCK : 3σ SN Ia(TRGB, Cep based on 2 anchors) PLANCK : 2σ 38
39 SN Ia(Cepheid based on 4 anchors) PLANCK : 3σ SN Ia(TRGB, Cep based on 2 anchors) PLANCK : 2σ 39
40 Our SN Ia(TRGB) estimate of H 0 : H 0 = 71.2 ±2.5 km/s/mpc Planck15 TIPSNU Riess+16 It agrees well with SN Ia (Cepheid based on the same anchors), supporting 2-3σ tension! SN Ia (Cepheid based on MW and M31) leads to a higher H0 value! Why? We need to improve the zero point accuracy of the TRGB and Cepheids, to determine a more accurate value of H 0 in the future. H 0 Any need for new physics?
41 (1) CCHP (Carnegie-Chicago H 0 Project) -Calibration of SN Ia using Pop II candles with HST Cycle 22 (PI: Freedman) -12 galaxies at <30 Mpc hosting SN Ia (2) Extension to NIR: JWST 41
42 -The TRGB is a secondary distance indicator based on geometric anchors, being an excellent tool for H 0! H 0 (TRGB-SN Ia) = ±2.50 (3.5% error), showing 2σ Hubble tension. -H 0 in 2018 is still evolving! -The future of the H 0 tension? -Stay tuned! 42
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