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MGR li (J i t ALMA Ob t / ESO) A J Ad (G i i Ob t )BJMCll M G Rawlings (Joint ALMA Observatory / ESO) A J Adamson (Gemini Observatory) B J McCall M. G. Rawlings (Joint ALMA Observatory / ESO), A. J. Adamson (Gemini Observatory), B. J. McCall (University of Illinois at Urbana-Champaign) & T H Kerr (UKIRT / Joint Astronomy Centre Hawaii) (University of Illinois at Urbana-Champaign) & T. H. Kerr (UKIRT / Joint Astronomy Centre, Hawaii) S Summary Summary Summary Summary Since Since their their initial initial detection detection by by Heger Heger in in 1922 1922, the the identification identification of of the the carriers carriers of of the the Since Since their their initial initial detection detection by by Heger Heger in in 1922 1922, the the identification identification of of the the carriers carriers of of the the Diff se Diff se Interstellar Interstellar Bands Bands (DIBs) (DIBs) has has gone gone on on to to become become one one of of the the longest longest Diffuse Diffuse Interstellar Interstellar Bands Bands (DIBs) (DIBs) has has gone gone on on to to become become one one of of the the longest longest- standing standing problems problems in in astrophysics astrophysics with with several several hundred hundred DIBs DIBs now now having having been been standing standing problems problems in in astrophysics, astrophysics, with with several several hundred hundred DIBs DIBs now now having having been been detected detected at at visual visual wavelengths wavelengths. Although Although the the carriers carriers are are widely widely thought thought to to be be detected detected at at visual visual wavelengths wavelengths. Although Although the the carriers carriers are are widely widely thought thought to to be be carbonaceo s carbonaceo s molec les/ions molec les/ions an an nambig o s nambig o s carrier carrier identification identification for for most most of of the the carbonaceous carbonaceous molecules/ions, molecules/ions, an an unambiguous unambiguous carrier carrier identification identification for for most most of of the the bands bands remains remains elusive elusive One One strong strong observational observational constraint constraint on on the the nature nature of of the the bands bands remains remains elusive elusive. One One strong strong observational observational constraint constraint on on the the nature nature of of the the carriers, carriers, however, however, is is the the detection detection of of DIB DIB substructure substructure via via high high-resolution resolution echelle echelle carriers, carriers, however, however, is is the the detection detection of of DIB DIB substructure substructure via via high high resolution resolution echelle echelle spectroscop spectroscop spectroscopy spectroscopy . In In addition addition to to the the many many visual visual DIBs DIBs found, found, two two DIB DIB detections detections were were reported reported in in the the In In addition addition to to the the many many visual visual DIBs DIBs found, found, two two DIB DIB detections detections were were reported reported in in the the near near infrared infrared b Joblin Joblin et et al al (1990 1990) near near 11797 11797 5 and and 13175 13175 A These These remain remain the the near near-infrared infrared by by Joblin Joblin et et al al. (1990 1990), ), near near 11797 11797.5 and and 13175 13175 A. These These remain remain the the longest longest-wavelength wavelength DIBs DIBs observed observed and and consequently consequently have have further further implications implications for for longest longest-wavelength wavelength DIBs DIBs observed, observed, and and consequently consequently have have further further implications implications for for the the nature nature of of the the carriers carriers. Despite Despite this, this, there there have have been been few few follow follow-up up observations observations the the nature nature of of the the carriers carriers. Despite Despite this, this, there there have have been been few few follow follow up up observations observations of of these these DIBs DIBs We We present present here here high high resol tion resol tion UKIRT UKIRT echelle echelle spectroscop spectroscop of of the the of of these these DIBs DIBs. We We present present here here high high-resolution resolution UKIRT UKIRT echelle echelle spectroscopy spectroscopy of of the the two two NIR NIR DIBs DIBs Detections Detections towards towards sightlines sightlines exhibiting exhibiting a range range of of visual visual extinctions extinctions two two NIR NIR DIBs DIBs. Detections Detections towards towards sightlines sightlines exhibiting exhibiting a range range of of visual visual extinctions extinctions are are presented, presented, and and variations variations in in the the properties properties and and profile profile shapes shapes of of the the bands bands are are are are presented, presented, and and variations variations in in the the properties properties and and profile profile shapes shapes of of the the bands bands are are considered considered in in the the conte t conte t of of the the kno n kno n properties properties of of the the narro narro optical optical DIBs DIBs considered considered in in the the context context of of the the known known properties properties of of the the narrow narrow optical optical DIBs DIBs. Ob i Ob i Observations Observations Observations Observations UKIRT UKIRT / CGS CGS4 echelle echelle observations observations at at 11797 11797 5 & UKIRT UKIRT / CGS CGS4 echelle echelle observations observations at at 11797 11797.5 & Å th th t I R 13175 13175 Å - August August 9 th th - 21 21 st st , 2008 2008. 1-pixel pixel width width slit slit I R 13175 13175 Å August August 9 21 21 , 2008 2008. 1 pixel pixel width width slit slit (0 6”) ”) of of 91 91 5” was was used used 2 × 2 sampling sampling used used with with (0.6”) ”) of of 91 91.5” was was used used. 2 × 2 sampling sampling used used with with non non-destructive destructive readout readout R ~ 37000 37000 V B non non-destructive destructive readout readout. R ~ 37000 37000. V B Targets Targets Targets Targets Sgr Sgr : “single “single cloud” cloud” sightline sightline Sgr Sgr : single single cloud cloud sightline sightline • Monitoring Monitoring of of HD HD 204827 204827 Monitoring Monitoring of of HD HD 204827 204827 C OB OB2 N 12 12 tt i l tt i l i htli i htli • Cyg Cyg OB OB2 No No. 12 12: prototypical prototypical sightline sightline • Eight Eight other other heavily heavily reddened reddened (above (above right) right) early early Examples of the UKIRT/CGS4 echelle NIR DIB • Eight Eight other other heavily heavily-reddened reddened (above (above right) right) early early- Examples of the UKIRT/CGS4 echelle NIR DIB t bt i d Th S i htli h type type stars stars (Stephenson (Stephenson 1992 1992) exhibiting exhibiting very very high high A V spectra obtained. The Sgr sightline was chosen type type stars stars (Stephenson, (Stephenson, 1992 1992) exhibiting exhibiting very very high high A V (6 6 15 15 8) d t diff diff ISM ISM (R li (R li t l 2000 2000 as a “single cloud” sightline and Cyg OB2 No 12 (6.6 - 15 15.8) due due to to diffuse diffuse ISM ISM (Rawlings (Rawlings et et al al. 2000 2000, as a single cloud sightline, and Cyg OB2 No. 12 Rawlings Rawlings et et al al 2003 2003) and and strong strong DIBs DIBs (right) (right) is the prototypical bright early-type star with very Rawlings Rawlings et et al al. 2003 2003) and and strong strong DIBs DIBs (right) (right). is the prototypical bright early type star with very hi h diff di ti ti high diffuse medium extinction. Equivalent widths Equivalent widths / Equivalent widths Equivalent widths / 2 5E-04 A 2 5E 05 Initial Res lts & Concl sions Initial Res lts & Concl sions 2.5E 04 A V 2.5E-05 Initial Results & Conclusions Initial Results & Conclusions Initial Results & Conclusions Initial Results & Conclusions 2 0E 04 2.0E-04 2.0E-05 • The The NIR NIR DIBs DIBs appear appear to to be be reasonably reasonably well well • The The NIR NIR DIBs DIBs appear appear to to be be reasonably reasonably well well fitted fitted by by a single single Gaussian Gaussian with with some some evidence evidence of of 1.5E-04 1.5E-05 fitted fitted by by a single single Gaussian, Gaussian, with with some some evidence evidence of of l l th l th i a long long-wavelength wavelength wing wing. 1.0E-04 1.0E-05 • Neither Neither (narrow) (narrow) band band shows shows complex complex 1.0E 04 • Neither Neither (narrow) (narrow) band band shows shows complex complex substructure, substructure, contrasting contrasting with with some some of of the the narrow narrow 5 0E 05 5 0E-06 substructure, substructure, contrasting contrasting with with some some of of the the narrow narrow ti l ti l DIB DIB ( S t l 1995 1995) 5.0E-05 5.0E 06 optical optical DIBs DIBs (e (e.g. Sarre Sarre et et al al. 1995 1995). 0 0E+00 • Per Per unit unit extinction extinction there there is is no no strong strong correlation correlation 0.0E+00 0.0E+00 Per Per unit unit extinction, extinction, there there is is no no strong strong correlation correlation bt bt th th 13175 13175 Å d 11797 11797 Å DIB DIB t th t th 0E+00 2E-05 4E-05 6E-05 8E-05 0E+00 5E-06 1E-05 2E-05 between between the the 13175 13175 Å and and 11797 11797 Å DIB DIB strengths strengths. W [11797 5 Å] W [11797 5 Å] / A W [11797.5 Å] W [11797.5 Å] / A V E i l t idth f th NIR DIB Th lt th i hti di t th b f Equivalent widths of the NIR DIBs. The plot on the right indicates the absence of a strong correlation on a per unit extinction basis Future Work Future Work strong correlation on a per -unit-extinction basis. Future Work Future Work • Check Check for for (anti (anti-)correlations )correlations against against other other DIBs DIBs Rf Rf Check Check for for (anti (anti )correlations )correlations against against other other DIBs DIBs d i ( 3 4 ) i th th bj t bj t References References and and organics organics (e (e.g. 3.4 m) m) in in the the same same objects objects. • Heger, Heger, M. L., 1922 1922, Lick Lick Observatory Observatory Bulletin, Bulletin, 10 10, No No. 337 337, 146 146 • Modelling Modelling of of carriers carriers • Joblin, C., D'Hendecourt, L., Leger, A. & Maillard, J. P. 1990 1990, Nature, Nature, 346 346, 729 729 • Modelling Modelling of of carriers carriers. • Rawlings, Rawlings, M. G., Adamson, Adamson, A. J. & Whittet, Whittet, D. C. B. 2003 2003, MNRAS, MNRAS, 341 341, 1121 1121 A l i A l i f HD HD 204827 204827 it i it i dt dt • Rawlings, Rawlings, M. G. Adamson, Adamson, A. J. & Whittet, Whittet, D. C. B. 2000 2000, ApJS, ApJS, 131 131, 531 531 • Analysis Analysis of of HD HD 204827 204827 monitoring monitoring data data. • Sarre, Sarre, P . J., Miles, Miles, J. R., Kerr, Kerr, T . H., Hibbins, Hibbins, R. E. & Somerville, Somerville, W . B. 1995 1995, MNRAS, MNRAS, 277 277L, L, 41 41S St h St h C B 1992 1992 AJ AJ 103 103 263 263 • Stephenson, Stephenson, C. B. 1992 1992, AJ, AJ, 103 103, 263 263

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Page 1: MGR li (JitALMAOb t /ESO)AJAd (G iiOb t )BJMCllM G ...bjm.scs.illinois.edu/posters/Rawlings2011.pdf · Title: Microsoft PowerPoint - Toledo_2011_DIBs_poster_final [Compatibility Mode]

M G R li (J i t ALMA Ob t / ESO) A J Ad (G i i Ob t ) B J M C llM G Rawlings (Joint ALMA Observatory / ESO) A J Adamson (Gemini Observatory) B J McCallM. G. Rawlings (Joint ALMA Observatory / ESO), A. J. Adamson (Gemini Observatory), B. J. McCall (University of Illinois at Urbana-Champaign) & T H Kerr (UKIRT / Joint Astronomy Centre Hawaii)(University of Illinois at Urbana-Champaign) & T. H. Kerr (UKIRT / Joint Astronomy Centre, Hawaii)

SSSummarySummarySummarySummary

SinceSince theirtheir initialinitial detectiondetection byby HegerHeger inin 19221922,, thethe identificationidentification ofof thethe carrierscarriers ofof thetheSinceSince theirtheir initialinitial detectiondetection byby HegerHeger inin 19221922,, thethe identificationidentification ofof thethe carrierscarriers ofof thetheDiff seDiff se InterstellarInterstellar BandsBands (DIBs)(DIBs) hashas gonegone onon toto becomebecome oneone ofof thethe longestlongestDiffuseDiffuse InterstellarInterstellar BandsBands (DIBs)(DIBs) hashas gonegone onon toto becomebecome oneone ofof thethe longestlongest--( )( ) gg ggstandingstanding problemsproblems inin astrophysicsastrophysics withwith severalseveral hundredhundred DIBsDIBs nownow havinghaving beenbeenstandingstanding problemsproblems inin astrophysics,astrophysics, withwith severalseveral hundredhundred DIBsDIBs nownow havinghaving beenbeendetecteddetected atat visualvisual wavelengthswavelengths.. AlthoughAlthough thethe carrierscarriers areare widelywidely thoughtthought toto bebedetecteddetected atat visualvisual wavelengthswavelengths.. AlthoughAlthough thethe carrierscarriers areare widelywidely thoughtthought toto bebecarbonaceo scarbonaceo s molec les/ionsmolec les/ions anan nambig o snambig o s carriercarrier identificationidentification forfor mostmost ofof thethecarbonaceouscarbonaceous molecules/ions,molecules/ions, anan unambiguousunambiguous carriercarrier identificationidentification forfor mostmost ofof thetheggbandsbands remainsremains elusiveelusive OneOne strongstrong observationalobservational constraintconstraint onon thethe naturenature ofof thethebandsbands remainsremains elusiveelusive.. OneOne strongstrong observationalobservational constraintconstraint onon thethe naturenature ofof thethecarriers,carriers, however,however, isis thethe detectiondetection ofof DIBDIB substructuresubstructure viavia highhigh--resolutionresolution echelleechellecarriers,carriers, however,however, isis thethe detectiondetection ofof DIBDIB substructuresubstructure viavia highhigh resolutionresolution echelleechellespectroscopspectroscopspectroscopyspectroscopy..p pyp py

InIn additionaddition toto thethe manymany visualvisual DIBsDIBs found,found, twotwo DIBDIB detectionsdetections werewere reportedreported inin thetheInIn additionaddition toto thethe manymany visualvisual DIBsDIBs found,found, twotwo DIBDIB detectionsdetections werewere reportedreported inin thethenearnear infraredinfrared bb JoblinJoblin etet alal ((19901990)) nearnear 1179711797 55 andand 1317513175 AA TheseThese remainremain thethenearnear--infraredinfrared byby JoblinJoblin etet alal.. ((19901990),), nearnear 1179711797..55 andand 1317513175 AA.. TheseThese remainremain thetheyy (( ))longestlongest--wavelengthwavelength DIBsDIBs observedobserved andand consequentlyconsequently havehave furtherfurther implicationsimplications forforlongestlongest--wavelengthwavelength DIBsDIBs observed,observed, andand consequentlyconsequently havehave furtherfurther implicationsimplications forforthethe naturenature ofof thethe carrierscarriers.. DespiteDespite this,this, therethere havehave beenbeen fewfew followfollow--upup observationsobservationsthethe naturenature ofof thethe carrierscarriers.. DespiteDespite this,this, therethere havehave beenbeen fewfew followfollow upup observationsobservationsofof thesethese DIBsDIBs WeWe presentpresent herehere highhigh resol tionresol tion UKIRTUKIRT echelleechelle spectroscopspectroscop ofof thetheofof thesethese DIBsDIBs.. WeWe presentpresent herehere highhigh--resolutionresolution UKIRTUKIRT echelleechelle spectroscopyspectroscopy ofof thethepp gg p pyp pytwotwo NIRNIR DIBsDIBs DetectionsDetections towardstowards sightlinessightlines exhibitingexhibiting aa rangerange ofof visualvisual extinctionsextinctionstwotwo NIRNIR DIBsDIBs.. DetectionsDetections towardstowards sightlinessightlines exhibitingexhibiting aa rangerange ofof visualvisual extinctionsextinctionsareare presented,presented, andand variationsvariations inin thethe propertiesproperties andand profileprofile shapesshapes ofof thethe bandsbands areareareare presented,presented, andand variationsvariations inin thethe propertiesproperties andand profileprofile shapesshapes ofof thethe bandsbands areareconsideredconsidered inin thethe conte tconte t ofof thethe kno nkno n propertiesproperties ofof thethe narronarro opticaloptical DIBsDIBsconsideredconsidered inin thethe contextcontext ofof thethe knownknown propertiesproperties ofof thethe narrownarrow opticaloptical DIBsDIBs..p pp p pp

Ob iOb i

ObservationsObservationsObservationsObservations

UKIRTUKIRT // CGSCGS44 echelleechelle observationsobservations atat 1179711797 55 &&UKIRTUKIRT // CGSCGS44 echelleechelle observationsobservations atat 1179711797..55 &&ÅÅ thth tt I R

1317513175 ÅÅ -- AugustAugust 99thth -- 2121stst,, 20082008.. 11--pixelpixel widthwidth slitslitI R

1317513175 ÅÅ AugustAugust 99 2121 ,, 20082008.. 11 pixelpixel widthwidth slitslit((00 66”)”) ofof 9191 55”” waswas usedused 22 ×× 22 samplingsampling usedused withwith

((00..66”)”) ofof 9191..55”” waswas usedused.. 22 ×× 22 samplingsampling usedused withwith(( )) ggnonnon--destructivedestructive readoutreadout RR ~~ 3700037000 V Bnonnon--destructivedestructive readoutreadout.. RR ~~ 3700037000.. V B

TargetsTargetsTargetsTargets gg

SgrSgr :: “single“single cloud”cloud” sightlinesightline SgrSgr :: singlesingle cloudcloud sightlinesightline•• MonitoringMonitoring ofof HDHD 204827204827MonitoringMonitoring ofof HDHD 204827204827

CC OBOB22 NN 1212 t t i lt t i l i htlii htli•• CygCyg OBOB22 NoNo.. 1212:: prototypicalprototypical sightlinesightlineygyg p ypp yp gg•• EightEight otherother heavilyheavily reddenedreddened (above(above right)right) earlyearly Examples of the UKIRT/CGS4 echelle NIR DIB•• EightEight otherother heavilyheavily--reddenedreddened (above(above right)right) earlyearly-- Examples of the UKIRT/CGS4 echelle NIR DIB

t bt i d Th S i htli htypetype starsstars (Stephenson(Stephenson 19921992)) exhibitingexhibiting veryvery highhigh AAVV spectra obtained. The Sgr sightline was chosen typetype starsstars (Stephenson,(Stephenson, 19921992)) exhibitingexhibiting veryvery highhigh AAVV

((66 66 1515 88)) dd tt diffdiff ISMISM (R li(R li tt ll 20002000p g g

as a “single cloud” sightline and Cyg OB2 No 12((66..66 -- 1515..88)) duedue toto diffusediffuse ISMISM (Rawlings(Rawlings etet alal.. 20002000,, as a single cloud sightline, and Cyg OB2 No. 12 (( )) ( g( g ,,RawlingsRawlings etet alal 20032003)) andand strongstrong DIBsDIBs (right)(right) is the prototypical bright early-type star with veryRawlingsRawlings etet alal.. 20032003)) andand strongstrong DIBsDIBs (right)(right).. is the prototypical bright early type star with very

hi h diff di ti tihigh diffuse medium extinction.gEquivalent widths Equivalent widths / Equivalent widths Equivalent widths /

2 5E-04 A2 5E 05

Initial Res lts & Concl sionsInitial Res lts & Concl sions2.5E 04 AV2.5E-05

Initial Results & ConclusionsInitial Results & ConclusionsInitial Results & ConclusionsInitial Results & Conclusions2 0E 042.0E-04 2.0E-05

•• TheThe NIRNIR DIBsDIBs appearappear toto bebe reasonablyreasonably wellwell•• TheThe NIRNIR DIBsDIBs appearappear toto bebe reasonablyreasonably wellwellfittedfitted byby aa singlesingle GaussianGaussian withwith somesome evidenceevidence ofof1.5E-04 1.5E-05 fittedfitted byby aa singlesingle Gaussian,Gaussian, withwith somesome evidenceevidence ofof

ll l thl th iiaa longlong--wavelengthwavelength wingwing..gg gg gg1.0E-04 1.0E-05

•• NeitherNeither (narrow)(narrow) bandband showsshows complexcomplex1.0E 04

•• NeitherNeither (narrow)(narrow) bandband showsshows complexcomplexsubstructure,substructure, contrastingcontrasting withwith somesome ofof thethe narrownarrow5 0E 05 5 0E-06 substructure,substructure, contrastingcontrasting withwith somesome ofof thethe narrownarrow

ti lti l DIBDIB (( SS tt ll 19951995))5.0E-05 5.0E 06

opticaloptical DIBsDIBs (e(e..gg.. SarreSarre etet alal.. 19951995))..pp (( gg ))0 0E+00

•• PerPer unitunit extinctionextinction therethere isis nono strongstrong correlationcorrelation0.0E+00 0.0E+00PerPer unitunit extinction,extinction, therethere isis nono strongstrong correlationcorrelation

b tb t thth 1317513175 ÅÅ dd 1179711797 ÅÅ DIBDIB t tht th0E+00 2E-05 4E-05 6E-05 8E-05 0E+00 5E-06 1E-05 2E-05

betweenbetween thethe 1317513175 ÅÅ andand 1179711797 ÅÅ DIBDIB strengthsstrengths..W [11797 5 Å] W [11797 5 Å] / A ggW [11797.5 Å] W [11797.5 Å] / AV

E i l t idth f th NIR DIB Th l t th i ht i di t th b fEquivalent widths of the NIR DIBs. The plot on the right indicates the absence of a q p gstrong correlation on a per unit extinction basis Future WorkFuture Workstrong correlation on a per-unit-extinction basis. Future WorkFuture Work

•• CheckCheck forfor (anti(anti--)correlations)correlations againstagainst otherother DIBsDIBsR fR f CheckCheck forfor (anti(anti )correlations)correlations againstagainst otherother DIBsDIBsdd ii (( 33 44 )) ii thth bj tbj t

ReferencesReferencesandand organicsorganics (e(e..gg.. 33..44 m)m) inin thethe samesame objectsobjects..gg (( gg )) jj

•• Heger,Heger, MM.. LL..,, 19221922,, LickLick ObservatoryObservatory Bulletin,Bulletin, 1010,, NoNo.. 337337,, 146146

•• ModellingModelling ofof carrierscarriersg ,g , ,, ,, yy ,, ,, ,,

•• Joblin, C., D'Hendecourt, L., Leger, A. & Maillard, J. P. 19901990,, Nature,Nature, 346346,, 729729 •• ModellingModelling ofof carrierscarriers..•• Rawlings,Rawlings, MM.. GG..,, Adamson,Adamson, AA.. JJ.. && Whittet,Whittet, DD.. CC.. BB.. 20032003,, MNRAS,MNRAS, 341341,, 11211121

A l iA l i ff HDHD 204827204827 it iit i d td t•• Rawlings,Rawlings, MM.. GG.. Adamson,Adamson, AA.. JJ.. && Whittet,Whittet, DD.. CC.. BB.. 20002000,, ApJS,ApJS, 131131,, 531531

•• AnalysisAnalysis ofof HDHD 204827204827 monitoringmonitoring datadata..•• Sarre,Sarre, PP.. JJ..,, Miles,Miles, JJ.. RR..,, Kerr,Kerr, TT.. HH..,, Hibbins,Hibbins, RR.. EE.. && Somerville,Somerville, WW.. BB.. 19951995,, MNRAS,MNRAS, 277277L,L, 4141SSSt hSt h CC BB 19921992 AJAJ 103103 263263

yy gg•• Stephenson,Stephenson, CC.. BB.. 19921992,, AJ,AJ, 103103,, 263263

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