Multiwavelength studies of HESS J1825-137 of the ISM next to HESS - - PowerPoint PPT Presentation

Multiwavelength studies of HESS J1825-137 of the ISM next to HESS J1825–137 and preliminary results from other TeV source

Nanten meeting 2015

• F. Voisin

Overall: HESS J1825-137 and HESS J1826-130

◮ TeV source powered by

PSR J1826-1334

◮ Spin down power

˙ ESN=2.8×1036 erg.s−1 , pulsar period 101 ms and d∼ 4.0 ± 0.1 kpc

◮ τ= ˙ P 2P indicates a pulsar

characteristic age of τ ∼ 20 kyr

◮ Pulsar J1826-1256 Spin

down power ˙ ESN=4.9×1036 erg.s−1, pulsar period ∼ 100 ms and τ ∼ 14kyr (Abdo et al 2009)

140 120 100 80 60 40 18.480 18.460 18.440 18.420 18.400 18.380 18.360 18.340

• 12.80
• 13.00
• 13.20
• 13.40
• 13.60
• 13.80
• 14.00
• 14.20
• 14.40
• 14.60

HESS J1826-130

HESS Nanten

LS 5039 DEC RA

P1

HESSJ1825-137

P2

Excess count map of HESS J1825-137 from HESS. P1: PSR J1826-1334 P2: PSR J1826-1256. (Aharonian et al 2006)

◮ Covers ∼1 degree of the

galactic plane

◮ Asymmetry in the γ-ray

morphology due to the interaction between the progenitor SNR and the northern dense molecular cloud

◮ Energy dependent

morphology is suggesting a leptonic scenario (Aharonian et al 2006)

◮ What is the origin of

HESSJ1826-130 to the north?

HESS J1825-137 Energy morphology map Red - Total flux below 0.8 TeV Green - Total flux bewteen 0.8-2.5 TeV Blue - Total flux above 2.5 TeV(De Jager and Djannati ata¨ ı 2008)

Motivations

◮ Determine the nature of the HESS J1826-130 emission north

to HESS J1825-137:Hadronic or Leptonic?

◮ γ-ray emission over HESS J1826-130 overlaps with a giant

molecular cloud first observed by Lemi` ere et al (2004) .Origins from progenitor SNR, PWN?

◮ Pulsar hadronic wind theoretically expected and indirect

evidence seen (wisp structures) (e.g. Hoshino et al 1992, Gallant et al 1994, Gaensler et al 2002 )

◮ TeV hadronic emission possible from PWN (e.g. Amato et al

2003 and 2013, Horns et al 2007)

◮ Progenitor SNR as particle accelerator?

4 3.5 3 2.5 2 18.46 18.45 18.44 18.43 18.42 18.41

• 12.8
• 12.9
• 13.0
• 13.1
• 13.2
• 13.3
• 13.4
• 13.5

Right ascension Declination

Mopra CS(1-0)

CR5 P2 CR3 CR2 CR1 CR4

HESS J1825-137

P1 Mopra CS(1-0) 160 150 140 130 120 110 100 90 80 70 60 18.48 18.46 18.44 18.42 18.40 18.38 18.36

• 12.4
• 12.6
• 12.8
• 13.0
• 13.2
• 13.4
• 13.6
• 13.8
• 14.0
• 14.2
• 14.4

Right ascension Declination P2 CR3 CR2 CR1 CR6

HESS J1825-137

P1

Nanten CO(1-0)

Nanten CO(1-0) CR5 CR4 20 18 16 14 12 10 8 6 18.48 18.46 18.44 18.42 18.40 18.38 18.36

• 12.4
• 12.6
• 12.8
• 13.0
• 13.2
• 13.4
• 13.6
• 13.8
• 14.0
• 14.2
• 14.4

Right ascension Declination

GRS 13CO(1-0)

P2 CR3 CR2

HESS J1825-137

CR1 CR6 GRS 13CO(1-0)

HESS J1825-137 HESS J1825-137 HESS J1825-137 HESS J1825-137 HESS J1825-137

P1 CR5 CR4 3 2.5 2 1.5 1 18.46 18.45 18.44 18.43 18.42 18.41

• 12.8
• 12.9
• 13.0
• 13.1
• 13.2
• 13.3
• 13.4
• 13.5

Right ascension Declination NR1 NR2 NR3 P1 P2 NR4 NR5

Mopra NH3(1,1) HESS J1825-137

Mopra NH3(1,1)

K km/s K km/s

Integrated intensity map between vlsr:40-60 km/s , kinematic distance:3.6-4.3 kpc CR:Regions where CS(1-0),13CO(1-0),CO(1-0) are observed. NR:Regions where NH3 are also observed.

0.0 5.0 10.0 CO(1-0) CR2/NR2 0.0 1.0 2.0

Antenna Temperature TA (K)

13CO(1-0)

0.0 0.2 0.4 0.6 20 40 60 80

VLSR (km/s)

CS(1-0) 0.0 0.2 0.4 NH3(1,1) 0.0 0.1 0.2 NH3(2,2) 20 40 60 80 0.00 0.04 0.08

VLSR (km/s)

NH3(3,3) 0.0 5.0 10.0 15.0 20.0 CO(1-0) CR1/NR1 0.0 1.0 2.0

Antenna Temperature TA (K)

13CO(1-0)

0.0 0.1 0.2 0.3 20 40 60 80

VLSR (km/s)

CS(1-0) 0.00 0.10 NH3(1,1) 0.00 0.05 NH3(2,2) 20 40 60 80 0.00 0.02

VLSR (km/s)

NH3(3,3) 0.0 5.0 10.0 CO(1-0) CR4/NR4 0.0 1.0 2.0

Antenna Temperature TA (K)

13CO(1-0)

0.0 0.1 0.2 20 40 60 80

VLSR (km/s)

CS(1-0) 0.00 0.04 0.08 NH3(1,1) 0.00 0.02 0.04 NH3(2,2) 20 40 60 80 0.00 0.02 0.04

VLSR (km/s)

NH3(3,3) 0.0 5.0 10.0 CO(1-0) CR3/NR3 0.0 1.0 2.0 3.0

Antenna Temperature TA (K)

13CO(1-0)

0.0 0.4 0.8 20 40 60 80

VLSR (km/s)

CS(1-0) 0.0 0.1 0.2 NH3(1,1) 0.0 0.1 0.2 NH3(2,2) 20 40 60 80 0.00 0.04 0.08

VLSR (km/s)

NH3(3,3) 0.0 2.0 4.0 6.0 CO(1-0) CR5/NR5 0.0 0.5 1.0 1.5

Antenna Temperature TA (K)

13CO(1-0)

0.0 0.1 20 40 60 80

VLSR (km/s)

CS(1-0) 0.00 0.04 0.08 NH3(1,1) 0.00 0.05 NH3(2,2) 20 40 60 80 0.00 0.02 0.04

VLSR (km/s)

NH3(3,3) 0.0 5.0 10.0 CO(1-0) CR6/NR6 0.0 0.5 1.0 1.5

Antenna Temperature TA (K)

13CO(1-0)

0.0 0.1 0.2 0.3 20 40 60 80

VLSR (km/s)

CS(1-0) 0.00 0.02 NH3(1,1) 0.00 0.02 NH3(2,2) 20 40 60 80 0.00 0.02

VLSR (km/s)

NH3(3,3)

P1

Region CR1 in detail

18.427 18.420 18.413

• 13.15
• 13.20
• 13.25
• 13.30
• 13.35
• 13.40

CR1

H62alpha 45-65 km/s CS (1-0) 40-60 km/s NH3(1,1) 40-60 km/s UC HII g018.15-0.29 C9 C8 C7 C6 C5 C4 C3 C2 C1 P1

RA DEC

CR1

Integrated intensity in K (km/s) in CR1 CS(1-0) between 40-60 km/s NH3(1,1) between 40-60 km/s H62α between 45-65 km/s ◮ Overall H2 mass using XCO=2.0×1020cm−2(K km/s)−1 ∼

1×105 M⊙ with an average of ∼ 102 cm−3

◮ The CS and NH3 estimation of H2 Mass reveals ∼ 104 M⊙,

corresponding with the H2 mass estimated by Roman-Duval (2010).

◮ Some spatial separation between CS and NH3

CR1 Dynamic studies

18.426 18.424 18.422 18.420 18.418 18.416 18.414

• 13.20
• 13.22
• 13.24
• 13.26
• 13.28
• 13.30
• 13.32
• 13.34
• 13.36

CR1

P1 13CO(1-0) 55-60km/s 50-55km/s 45-50 km/s

RA DEC

CS(1-0)

CR1

0.0 1.0 2.0 3.0 4.0 13 14 15 16 17 18 0.0 1.0 2.0 3.0 4.0

Antenna Temperature TA (K)

19 20 21 22 23 24 0.0 1.0 2.0 3.0 4.0 25 26 27 28 29 30 0.0 1.0 2.0 3.0 4.0 31 32 33 34 35 36 0.0 1.0 2.0 3.0 4.0 45 50 55 60 r g b37 45 50 55 60 38 45 50 55 60 39 45 50 55 60 VLSR (km/s) 40 45 50 55 60 41 45 50 55 60 42 0.0 1.0 2.0 3.0 4.0 1 CS(1-0)x4 2 3

13CO(1-0)

4 5 6 0.0 1.0 2.0 3.0 4.0 7 8 9 10 11 12

CS(1-0) integrated intensity

• map. Box Averaged spectra
• verlaying the map. The

white dashed ellipse indicates CR1. Broad CS (1-0) and

13CO(1-0) emission (e.g

box 21). Emission varies greatly, changing from a single peak at vlsr ∼ 50 km/s (center of CR1) to double peak at ∼46-54 km/s (e.g box 34 and 23)

Spitzer

18.460 18.450 18.440 18.430 18.420 18.410 18.400 18.390

• 12.60
• 12.80
• 13.00
• 13.20
• 13.40
• 13.60

20 10 UC HII g018.15-0.29 Spitzer 5.8 micro Spitzer 24 micro Spitzer 8 micro CR5 P2 CR3 CR2 CR1 CR4 P1

RA DEC

CR1 indicates perturbation either coming from: → SNR → PWN → Shock from stars in the star-forming region ( e.g UCHII 18.15 -0.29 box 17 ) adding perturbations in its vicinity → Cloud-Cloud collision.

Supernova shock?

55 54 53 52 51 50 49 48 47 46 45 18.46 18.45 18.44 18.43 18.42 18.41 18.40

• 12.7
• 12.8
• 12.9
• 13.0
• 13.1
• 13.2
• 13.3
• 13.4
• 13.5

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

(h) (°) map vcent CO(1−0)

13 20 40 60 80 100 120 140 160 5000 10000 15000 20000 25000 30000 35000 40000 45000 0.5 1 1.5 2 rSNR (parsec) θ(degree) time(yr) n0=0.001 cm-3 5 10 15 20 25 30 5000 10000 15000 20000 25000 30000 35000 40000 45000 0.1 0.2 0.3 0.4 rSNR (parsec) θ(degree) time(yr) GMC n1 CR1 n2=400 cm-3 n0=0.001 cm-3 n1=100 cm-3 n1=10 cm-3

90 101 112 123 134 145 156 167 178 189 200 18.65 18.60 18.55 18.50 18.45 18.40 18.35 18.30 18.25 18.20 18.15

• 11.00
• 12.00
• 13.00
• 14.00
• 15.00
• 16.00
• 17.00

P2 P1 CR6

HESS J1826-130 DEC RA

CR1

HESS J1825-137

(°) (h) R

γ-ray prediction 1

Scenario 1

◮ Assume all high energy particles are confined inside the SN

shock.

◮ L100 GeV = R2

CR1

4d2

CR1

ηppESN τpp 2¯ n 4αK 1−α

π

κπd2

• 100 GeV

mp

2−α

◮ Assuming dCR1=20pc and RCR1=9pc n=400 cm−3 and α=2.2 ◮ L100 GeV = 7.3 × 10−11 n 400 cm−3 dCR1 28 pc

−2 erg cm2s−1 L100 GeV=2.12×10−12 erg cm−2 s−1.for HESS J1825-137 center: WAY TOO HIGH

x

SN origin d r CR1

CR1 CR1

γ-ray prediction 2

Scenario 1

◮ Assume all high energy particles escaped the high energy

particles escaped the SN shock.

◮ D (E) = D0

• E

10 GeV/

• B

3 µG ◮ r100 GeV ∼ 86

• B

3 µG

−1/4 pc

◮ L>100GeV ∼ 1.1 × 10−13 erg cm−2s−1

Uncertainties regarding the isotropic diffusion of TeV par- ticle and how much particles escaped the SNR

x

SN origin SN shock escaping CR CR1

HESS J1026-582

2.5e+03 2.7e+03 2.8e+03 3e+03 3.1e+03 3.3e+03 3.4e+03 3.6e+03 3.7e+03 3.9e+03 4e+03 284.80 284.70 284.60 284.50 284.40 284.30

• 0.20
• 0.30
• 0.40
• 0.50
• 0.60
• 0.70

HESS J1023-575 HESS J1026-582

SiO3 SiO2 SiO1 CS8 CS7 CS6 CS5 CS1 CS4 CS3 CS2 CS1 0.0 0.2 0.4 CS1 0.0 0.2 0.4

Antenna Temperature TA (K)

CS2 0.00 0.20 0.40

• 30
• 10

10 30 CS3 0.0 0.2 0.4 CS4 0.0 0.2 0.4

Antenna Temperature TA (K)

CS5 0.00 0.20 0.40

• 30
• 10

10 30 CS6 0.0 0.2 0.4 CS7 0.0 0.2 0.4

Antenna Temperature TA (K)

CS8 0.00 0.20 0.40

• 30
• 10

10 30 CS9 0.0 0.2 0.4 SiO1 0.0 0.2 0.4

Antenna Temperature TA (K)

SiO2 0.00 0.20 0.40

• 30
• 10

10 30 SiO3

HI 21cm integrated intensity v =0−30km/s

lsr

Spitzer 8 micro

MOST 843 micro

HESS J1026-582

1e+03 1.03e+03 1.05e+03 1.08e+03 1.1e+03 1.13e+03 1.15e+03 1.18e+03 1.2e+03 1.23e+03 1.26e+03 304.60 304.40 304.20 304.00 303.80 303.60 0.20 0.00

• 0.20
• 0.40
• 0.60

HESS J1303-631

PSR J1301-6305 CS2 CS1 0.0 0.2

Antenna Temperature TA (K)

CS1 0.0 0.2 10 30 50 70

VLSR (km/s)

CS2

21cm HI integated intensity v =28−37km/s

lsr 0.0781 0.0836 0.0891 0.0947 0.1 0.106 0.111 0.117 0.122 0.128 0.133 304.30 304.25 304.20 304.15 304.10 304.05 304.00 303.95 303.90 0.00

• 0.05
• 0.10
• 0.15
• 0.20
• 0.25
• 0.30
• 0.35
• 0.40

J303−631 rms map l b

Conclusion and future works

◮ Region CR1 shows interesting dynamics feature, its radius and

mass would allow γ-ray enhancement from cosmic-rays.

◮ Region CR1 nests several star forming regions. ◮ Excellent motivation to extend hard X-ray study to CR1.

(Anticorrelation Hard X-rays and dense gas). Future work:

◮ Detailed study of cloud cloud collision needed towards CR1. ◮ Modelling lepton and hadron induced γ-ray emission towards

HESS J1826-130.

Thanks for listening

backup slides

13CO Velocity Dispersion and Velocity Centroid

4 3.5 3 2.5 2 18.46 18.45 18.44 18.43 18.42 18.41 18.40

• 12.7
• 12.8
• 12.9
• 13.0
• 13.1
• 13.2
• 13.3
• 13.4
• 13.5

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4 13CO(1−0) Velocity dispersion map 55 54 53 52 51 50 49 48 47 46 45 18.46 18.45 18.44 18.43 18.42 18.41 18.40

• 12.7
• 12.8
• 12.9
• 13.0
• 13.1
• 13.2
• 13.3
• 13.4
• 13.5

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4

DEC RA

P2 CR3 CR2 CR1 P1 CR5 CR4 13CO(1−0) Velocity centroid map

(Left) 13CO(1-0) Velocity dispersion map. Black dashed contours: Integrated intensities above 10K km/s Black solid contours: above 20 K km/s HESS contours. (Right) GRS 13CO(1-0) velocity centroid map.

Spitzer and CS+GRS spectra

18.426 18.424 18.422 18.420 18.418 18.416 18.414

• 13.20
• 13.22
• 13.24
• 13.26
• 13.28
• 13.30
• 13.32
• 13.34
• 13.36

Spitzer

P1 13CO(1-0) 5.8 micro 8 micro 24 micro

R A DEC

CS(1-0)

CR1

0.0 1.0 2.0 3.0 4.0 13 14 15 16 17 18 0.0 1.0 2.0 3.0 4.0

Antenna Temperature TA (K)

19 20 21 22 23 24 0.0 1.0 2.0 3.0 4.0 25 26 27 28 29 30 0.0 1.0 2.0 3.0 4.0 31 32 33 34 35 36 0.0 1.0 2.0 3.0 4.0 45 50 55 60 r g b37 45 50 55 60 38 45 50 55 60 39 45 50 55 60 VLSR (km/s) 40 45 50 55 60 41 45 50 55 60 42 0.0 1.0 2.0 3.0 4.0 1 CS(1-0)x4 2 3

13CO(1-0)

4 5 6 0.0 1.0 2.0 3.0 4.0 7 8 9 10 11 12

Spitzer map overlaid by CS(1-0) + GRS 13CO(1-0) spectra.

Detailed view between 40-60 km/s with GRS

14 13 12 11 10 9 8 7 6 18.48 18.46 18.44 18.42 18.40 18.38 18.36

• 12.4
• 12.6
• 12.8
• 13.0
• 13.2
• 13.4
• 13.6
• 13.8
• 14.0
• 14.2
• 14.4

Right ascension Declination

13CO(1-0)

P2 CR3 CR2

HESS J1825-137

CR1 CR6 GRS 13CO(1-0)

HESS J1825-137 HESS J1825-137 HESS J1825-137 HESS J1825-137 HESS J1825-137

P1 CR5 CR4 8 7.5 7 6.5 6 5.5 18.48 18.46 18.44 18.42 18.40 18.38 18.36

• 12.4
• 12.6
• 12.8
• 13.0
• 13.2
• 13.4
• 13.6
• 13.8
• 14.0
• 14.2
• 14.4

Right ascension Declination

13CO(1-0)

P2 CR3 CR2

HESS J1825-137

CR1 CR6 GRS 13CO(1-0)

HESS J1825-137 HESS J1825-137 HESS J1825-137 HESS J1825-137 HESS J1825-137

P1 CR5 CR4

vlsr=45−60 km/s vlsr=40−45 km/s

13CO(1-0) integrated intensity map between 40-45 km/s and 45-60 km/s