wise properties of planetary nebulae from the dsh cataloguethe wide-field infrared survey explorer...

WISE properties of planetary nebulaefrom the DSH catalogue

M. Kronberger1,*, G. H. Jacoby2, D. Harmer3, D. Patchick1

APN VI, 2013/11/04 – 08, Playa del Carmen, Mexico

1 Deep Sky Hunters Collaboration

2 GMTO Corporation, 813 Santa Barbara St, Pasadena, CA 91101

3 NOAO, 950 N Cherry Ave, PO Box 26732, Tucson AZ 85726-6732

* email: [email protected]

Outline

APN VI, 2013/11/04 – 08, Playa del Carmen, MexicoM. Kronberger et al., WISE properties of PNe from the DSH catalogue

1. Introduction

2. WISE and planetary nebulae

3. WISE properties of DSH planetary nebulae

4. WISE as a tool of discovering new PNe

5. Special cases

6. Summary & Conclusions

The Deep Sky Hunters:

A group of (mostly) amateur astronomers hunting for unknown Deep Sky objects usingvarious resources (DSS, SDSS, WISE, 2MASS, VIZIER, ….)

• Foundation date: June 2003

• Number of members: 370

• Communication: via yahoo newsgroup (http://groups.yahoo.com/neo/groups/deepskyhunters/info)

• Emphasis: Initially on open clusters and other stellar aggregates …..

1. Introduction


UKIDSS

UKIDSS

UKIDSS

UKIDSS2MASS

Sup

erC

osm

os

Sky

Surv

eys

Sup

erC

osm

os

Sky

Surv

eys

Sup

erC

osm

os

Sky

Surv

eys

UKIDSS

UKIDSS

UKIDSS

UKIDSS

DSS

DSS

DSS

2MASS

The Deep Sky Hunters

• A group of (mostly) amateur astronomers hunting for unknown Deep Sky objects usingvarious resources (DSS, SDSS, WISE, 2MASS, VIZIER, ….)

• Foundation date: June 2003

• Number of members: 370

• Communication: via yahoo newsgroup (http://groups.yahoo.com/neo/groups/deepskyhunters/info)

• Emphasis: Initially on open clusters and other stellar aggregates …..

1. Introduction

UKIDSS

UKIDSS

UKIDSS

UKIDSS2MASS

Sup

erC

osm

os

Sky

Surv

eys

Sup

erC

osm

os

Sky

Surv

eys

Sup

erC

osm

os

Sky

Surv

eys

… However, something new came up in Oct 2003!

10″WIYN 3.5-m

Pa 1


Digitized Sky Survey


1. Introduction

Look out for PN-like objects

DSS-II B DSS-II R DSS-II NIR

Sup

erC

osm

os

Sky

Surv

eys

+ +

• publicly available Sky Surveys (mostly DSS)

• amateur [S II]-Hα-[O III] imagery

1

Contact Astronomers3

Get narrowband images

WIYN 3.5-mKPNO 2.1-mKPNO 4-mSPM 0.84-mOHP 1.2-m…WIYN 3.5-mHα

4

WIYN 3.5-mSAAO 1.9-mSPM 2.1-mOHP 1.2-m

WIYN 3.5-m

Validate candidates spectroscopically5

Check Databases2

The DSH PN candidate validation queue

http://www.google.at/url?sa=i&source=images&cd=&cad=rja&docid=kKki9TyA7IZjWM&tbnid=IUV1SZPj500hoM:&ved=0CAgQjRwwAA&url=http://cdsweb.u-strasbg.fr/logos.html&ei=Ui9xUrfjKsmctAaIn4CQCg&psig=AFQjCNHmDLlb8CGjC1ojnqcK5fTj4cofxg&ust=1383235794759395

http://www.google.at/url?sa=i&rct=j&q=&esrc=s&frm=1&source=images&cd=&cad=rja&docid=kKki9TyA7IZjWM&tbnid=BI_quqSpiHzD4M:&ved=0CAUQjRw&url=http://cdsweb.u-strasbg.fr/logos.html&ei=by9xUsPzDofVswbj34GYDw&bvm=bv.55617003,d.bGE&psig=AFQjCNEBuxOo-6WoevPu1nBTtjXgZPlEwA&ust=1383235820117583

http://www.google.at/url?sa=i&rct=j&q=&esrc=s&frm=1&source=images&cd=&cad=rja&docid=c5GB1k8sgqg-wM&tbnid=IBr388_v7En1TM:&ved=0CAUQjRw&url=http://ned.ipac.caltech.edu/&ei=ly9xUsCNNoTDtQaQt4CwDw&bvm=bv.55617003,d.bGE&psig=AFQjCNGMyAxTU71BuLibKpxCDXowiXtaqQ&ust=1383235859278581

http://www.google.at/url?sa=i&rct=j&q=&esrc=s&frm=1&source=images&cd=&cad=rja&docid=nNQEjsW7ergmWM&tbnid=OgciDLi8ZjzHiM:&ved=0CAUQjRw&url=http://cdsads.u-strasbg.fr/&ei=AzBxUsWiLMOBtAaiwoHoDA&bvm=bv.55617003,d.Yms&psig=AFQjCNHfNWkwCkLI06mbDRygSY3Jr9GmXg&ust=1383235919243697

CGPN 1

MASH-I 2 + MASH-II 3

IPHAS 4

DSH, true PNe 5-7

DSH, likely PNe 5,6,8

DSH, possible PNe

1. Introduction


Distribution of DSH PNe and candidates in the sky

1 L. Kohoutek, A&A 378, 843 (2000)2 Q. A. Parker et al., MNRAS 373, 79 (2006)3 B. Miszalski et al., MNRAS 384, 525 (2008)4 L. Sabin, this contribution

5 G. Jacoby et al., PASA 27, 156 (2010)6 M. Kronberger et al., IAUS 283, 414 (2012)7 D. Frew et al., in preparation8 M. Kronberger et al., poster B03, this contribution

0

30

60

90

120

possible and likelyPNe

spectroscopicallyobserved

confirmed PNe

# o

bje

cts

within MASH/IPHAS

outside MASH/IPHAS

0

50

100

150

200

250

candidates detected Hα/[O III] images taken

possible and likelyPNe

# o

bje

cts

within MASH/IPHAS

outside MASH/IPHAS


Most candidates located in areas complementaryto IPHAS and MASH

1. Introduction

Overall detection efficiency ≈ 60%

The DSH PN survey: current census


Technical data

• Mission period: 2010/01 –2011/02 (12 + 22um: 2010/01 - 2010/08)

• Bands: 3.4 um, 4.6 um, 12 um, 22 um

• angular resolution: 6.1“, 6.4“, 6.5“, 12.0“

• Sensitivities: < 0.08 mJy, 0.11 mJy, 1 mJy, 6 mJy 100x more sensitive than Akari and IRAS at these wavelengths!

Statistics

• >99% of the sky observed at least 2x in all bands

• Source catalogue: 563 million objects

http://wise2.ipac.caltech.edu/docs/release/allsky/figures/4band_cryo-w1-ach_equ-rh_crop.jpg

E. J. Wright et al., AJ 140, 1868 (2010)

Sky coveragePass bands


http://www.jpl.nasa.gov/news/news.php?feature=2183

http://irsa.ipac.caltech.edu/Missions/wise.html

The Wide-field Infrared Survey Explorer (WISE)



NGC 6445, ISO-SWSP. A.M. van Hoof, AJ 532, 384 (2000)

Where does the emission observed with WISE originate from?



NGC 6445, ISO-SWSP. A.M. van Hoof, AJ 532, 384 (2000)

Where does the emission observed with WISE originate from?

IRSA



Bernard-Salas, J. et al., ApJ 699, 1541 (2009)

[Ne III][S IV] [O IV]

Spitzer – IRS

Dust rich High-excitation

IRSA IRSA

• PNe considerably brighter in W3 & W4than in W1 & W2

• Dust-rich PNe usually brighter than high-excitation PNe

• W1+2: some line emission + CSPN, littlecontinuum

• W3: PAH + continuum, high-excitation lines

• W4: Continuum + some [O IV]

Sample constraints

• True and Likely PNe

• Location: outside of |b| = 5°

• Discovery method: visual surveying of DSS and SDSS images

„quasi-homogeneous sample“

3. DSH PNe: WISE properties


Sample properties

• Total number: 52 Objects

• All main morphological classes (A,B,E,I,R) represented

• Sizes: almost stellar to several arcminutes

• ≈ 25% spherical, uniform shells

0

5

10

15

20

0-30 arcsec 30-60 arcsec > 60 arcsec0

5

10

15

20

25

A B, B? E I R

Size distribution morphologies

Spherical PNe

Morphological classification in accordance with MASH catalogue (Q.A. Parker et al., MNRAS 373,79 (2006))

The WISE properties of medium-to-high Galactic latitude PNe were studied by a subsample of the DSH PN catalogue:


Asymmetric PNe (A,B,I)


Pa 5Kn 23 KnPa 1 Kn 12 Kn 26 Kn 10

Kn 25Te 11

Pa 13 Kn 64 Kn 59 Kn 58IRSA IRSA IRSA IRSA IRSA IRSA

IRSA IRSA IRSA IRSA IRSA IRSA

All fields 3‘×3‘, except Kn 64 (20‘×20‘)

R = W4G = W3B = W2



Elliptical PNe

Pa 15Kn 30 Kn 44 Kn 4 Kn 60 Kn 33

KTC 1Kn 50 Kn 56 Kn 41 Kn 21 Pa 12

Kn 39Pa 33 Kn 40 Kn 37 CGMW 4-2085 Fer 4

Kn 62Kn 2 Pa 11



IRSA IRSA IRSA



R = W4G = W3B = W2


Round, non-spherical PNe


Kn 42Kn 61 Pa 10Kn 24

IRSA IRSA IRSA IRSA


R = W4G = W3B = W2


Spherical PNe


Kn 36 Kn 5 Kn 31 Kn 1 Pa 14 Kn 16

Kn 63

Kn 13Kn 19 Kn 3 Pa 9 Kn 34 Kn 45

Kn 48

R = W4G = W3B = W2



IRSA IRSA

All fields 3‘×3‘, except Kn 45 and Kn 63 (10‘×10‘)


• Most asymmetric, elliptical and non-spherical round PNe are detected in WISE imagery

• Most spherical PNe are invisible on WISE imagery

0

5

10

15

20

0-30 arcsec 30-60 arcsec > 60 arcsec

0

5

10

15

20

25

A B, B? E I R

• Objects < 30“ almost entirely visiblein WISE

• Larger objects less likely to show up

3. DSH PNe: WISE properties – summary of results

Size distribution

morphologies

Spherical PNe

89%

63%53%

0%

100%

100%

100%

81%

14%

PNe with WISE detection

Comparison of DSH data with statistics for MASH PNe outside of |b| = 5°

3. DSH PNe: WISE properties – comparison with MASH PNe

Size # total % of WISE detections DSH sample

0-30 arcsec 133 90 % 89 %

30-60 arcsec 40 60 % 63 %

> 60 arcsec 42 38 % 53 %

Type # total % of WISE detections DSH sample

A 7 43 % (0 %)

B 14 64 % 100 %

E 106 81 % 81 %

I 2 100 % (100 %)

R, non-Sph 39 95 % 100 %

R, Sph 36 39 % 14 %

S 11 91 % -

Size dependence

Dependence on morphology

Very similar size dependence between MASH and DSH sample

Very good agreement for elliptical and non-spherical round PNe

Spherical PNe significantly less likely to be detected in WISE imagery


Brackets: only one object in sample

[W2-W3,W3-W4] colour-colour diagram:

DSH PNe: WISE properties – comparison with MASH PNe

DSH sample


-1

0

1

2

3

4

5

6

-1 0 1 2 3 4 5 6 7

W3

-W4

W2-W3

A,B,IERSph

• Only objects with clear detections in W3 or W4

• Multiple detections possible (especially forobjects > 30“)

„PN-bulk“

• Only objects with clear detections in W3 or W4

• Multiple detections possible (especially forobjects > 30“)

DSH PNe: WISE properties – comparison with MASH PNe

MASH sample


-1

0

1

2

3

4

5

6

-1 0 1 2 3 4 5 6 7

W3

-W4

W2-W3

A,B,IERSphS

No fundamental (photometric) differences between different PN types, but large scatterin the data!

[W2-W3,W3-W4] colour-colour diagram:

„PN-bulk“


4. WISE as a tool for discovering new PNe

Parker , Q. A. et al., IAUS 283, 9 (2012):

Mid-IR data can be a powerful toolto discover new PNe!

• WISE survey for new PN candidates started outside of the MASH and IPHAS surveyareas

• Project mostly followed up by D. Patchick

• Strategy: Combining WISE with DSS imagery to look for poss. CSPN + nebulosity

KPNO 2.1-m KPNO 2.1-m KPNO 2.1-m KPNO 2.1-m

KPNO 2.1-m

KPNO 2.1-m

KPNO 2.1-m

KPNO 2.1-m

KPNO 2.1-m

4. WISE as a tool for discovering new PNe

KPNO 2.1-m

KPNO 2.1-m

See also poster B03!

Preliminary results

• ≈ 25 new possible and likely PNe detected

• Sizes: almost stellar objects to several arcmin

• Many rings and asymmetric PNe, sphericalobjects clearly underrepresented


Kn 59

5. Special cases

• High-Galactic latitude object ( b = +25.45°)

• PN-like, Medium-excitation spectrum

• Morphology:

SDSS, Sloan-g

SPM 0.84-m

1'


L. Sabin, SPM 2.1-m

• small, bright core 4“x4“

• halo 228“x174“ with multipolar characteristics

Kn 59

5. Special cases

• High-Galactic latitude object ( b = +25.45°)

• PN-like, Medium-excitation spectrum

• Morphology:

SDSS, Sloan-g

SPM 0.84-m

1'


SPM 2.1-m

• small, bright core 4“x4“

• halo 228“x174“ with multipolar characteristics

WISE-characteristics:

No emission detectedat 22um!

W1 W2

W3 W4

PN

?

?

IRSA IRSA

IRSA IRSA


Te 11

5. Special cases

• PN spectrum but very peculiar morphology

• Strong ISM interaction, poss with Barnards‘ Loop

• CS: fairly red, eclipsing binary

• PN or symbiotic star?

B. Miszalski et al., APN V, 328 (2011)

p = 0.12d

WIYN 3.5-mHα + [O III] + [O III]

WIYN 3.5-m

WIYN 3.5-mHα + [O III] + [O III]

APN Ve, 2013/11/04 – 08, Playa del Carmen, MexicoM. Kronberger et al., WISE properties of PNe from the DSH catalogue

Te 11

5. Special cases

• PN spectrum but very peculiar morphology

• Strong ISM interaction, poss with Barnards‘ Loop

• CS: fairly red, eclipsing binary

• PN or symbiotic star?

B. Miszalski et al., APN V, 328 (2011)

p = 0.12d

WISE-characteristics:

W1 W2

W3 W4

Again, no emission at 22um

PN

?

?

IRSA IRSA

IRSA IRSA

5. Special cases

Pa 19 & Pa 30

• Located within IPHAS survey area

• characteristics:

• W4-bright

• blue CS (DSS):

• Pa 19: B ~ 17.2, B-R ≈ -0.2

• Pa 30: B ~ 15.5, B-R ≈ -0.3

Low reddening


KPNO 2.1-m Hα + [O III] images taken June - October 2013

• No nebulosity on IPHAS imagery

faint shells dominated by [O III] emission

PNe

?

?

Pa 30

Pa 19

IPHASX J190512.4+161347 IRSA

IRSA

5. Special cases

Pa 19 & Pa 30

• Located within IPHAS survey area

• characteristics:

• W4-bright

• blue CS (DSS):

• Pa 19: B ~ 17.2, B-R ≈ -0.2

• Pa 30: B ~ 15.5, B-R ≈ -0.3

Low reddening


KPNO 2.1-m Hα + [O III] images taken June - October 2013

• No nebulosity on IPHAS imagery

faint shells dominated by [O III] emission

PNe

?

?

Pa 30

Pa 19

IPHASX J190512.4+161347

Hα

+ [O

III]

+ [

O II

I]

[O III]

KPN

O 2

.1-m

KPNO 2.1-m

Pa 30

Pa 19

IPHASX J190512.4+161347

6. Summary and conclusions


• The WISE properties of a subsample of the DSH True and Probable PNe were studied.

• Results:

• Larger PNe are less likely to have a WISE detection than smaller PNe

• elliptical, non-spherical round, and asymmetric PNe: Similar detection probabilities and photometric properties

• Spherical shells are significantly less often detected than all other PN types

• 25 new PN candidates detected in a directed survey of the Milky Way using WISE imagery, many of them without optical counterpart on DSS, IPHAS or MASH

WISE is an excellent all-sky tool to detect new PNe and to reveal possible mimics

Not all PNe detectable with optical methods will show up also in WISE!

Acknowledgments


This research has made use of:

• the NASA/IPAC Infrared Science Archive, which is operated by the Jet PropulsionLaboratory, California Institute of Technology, under contract with the NationalAeronautics and Space Administration.

• data products from the Wide-field Infrared Survey Explorer, which is a joint project ofthe University of California, Los Angeles, and the Jet Propulsion Laboratory/CaliforniaInstitute of Technology, funded by the National Aeronautics and Space Administration.

• data products from the Two Micron All Sky Survey, which is a joint project of theUniversity of Massachusetts and the Infrared Processing and Analysis Center/CaliforniaInstitute of Technology, funded by the National Aeronautics and Space Administrationand the National Science Foundation.

• the VizieR catalogue access tool and the SIMBAD database, operated at CDS,Strasbourg, France.

• data obtained from the SuperCOSMOS Science Archive, prepared and hosted by theWide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which isfunded by the UK Science and Technology Facilities Council.

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