! FoP.l Nc · 2020. 3. 17. · the same ultraviolet system (Rountree & Sonnebom 1993, Paper II). In...

NASA--] Reference NASA-RP-131219930022548

Publication'] 1312 ....................................................

....1 August 1993

-1 Spectral Classification With the] InternationalUltravioletExplorer:

] AnAtlas of B-TypeSpectra

1

• Janet Rountree and

] George Sonnebom _t,'GL_RES_RCHC_i':_LIBRARYNAS_HAMPTON,V/_RGIIilA

l

! FoP.l___Nc_

....

._1

__]

https://ntrs.nasa.gov/search.jsp?R=19930022548 2020-03-17T05:07:03+00:00Z

IMA

SA

The

1981C

onference

On

Rem

ote

Sen

sing

Ed

ucatio

nM

ay18-22,

1981S

ession

ST

AF

FN

EE

DS

FO

RE

FF

EC

TIV

ER

EM

OT

ESE

NS

ING

EX

PLO

RA

TIO

N

byJam

esR

.D

avisP

hillipsP

etroleumC

ompany

Bartlesville,

Oklahom

a

Rem

otesensing

isassum

inga

role

inthe

searchfo

rnatural

resources.R

esearchhas

shown

thatsatellite

imagery

may

beim

portantin

locatingcertain

typesof

petroleumand

mineral

deposits.

Either

director

indirectindications

ofnatural

resourceoccurrences

haveto

bedetectibl,

fromstandard

orenhanced

imagery

data.T

heseindications

arethe

resultof

geochemical

alterationof

_oilsor

geochemical

stresson

vegetationin

affectedareas

ascom

paredto

thesurrounding

unaffectedarea.

Traditional

mapping

ofgeological

structurecan

beaccom

plishedusing

satelliteim

agerydata.

Inpetroleum

explorationthis

may

behelpful

inrem

oteunderdeveloped

countries,but

probablyw

illnot

beutilized

extensivelyin

well

mapped

areassuch

asthe

U.

S.,

Canada,

andE

urope.

Inthe

caseof

petroleum,

itis

generallyaccepted

thatpetroleum

migrates

tothe

surfacew

hereit

caninteract

geochemically

andgeobotanically.

Petroleum

rangingfrom

asphaltto

methane

isencountered

asseeps

orm

icroseepsin

soilsabove

petroleumtrapped

atdepth.

To

nalano

malies

have

beenrepo

rtedo

nLandsat

imagery,

for

example,

fromW

yom

ing.It

isbelieved

thatiron

depletionand

thepresence

ofhydrocarbons

inthe

soilover

theP

atrickD

rawfield

may

bethe

causeof

thestressed

sagebrushat

thatlocation

(N.

L.F

roman,

1976and

R.

W.

Marrs

andR

.G

aylord,1981).

At

otherlocations

suchanom

alieshave

beenattributed

todevelopm

entroads

andw

elllocations

developedafter

thediscovery

ofan

oilfield.

Tonal

anomalies

inRailroad

Valley,

Nevada

providean

interestingcase

forthe

useof

enhancedim

ageryto

clarifyan

anomaly.

Oil

was

discoveredin

theE

oceneat

4000feet

belowthe

valleyfloor.

The

anomalies

donot

coincidew

iththe

outlineof

theknow

nproduction.

This

casew

ouldprovide

agood

caseto

investigateboth

geochemically

andgeobotanically.

34

.].,,s, I][I]@iililini][ll]I

•] Reference 31176014046131Publication

] 1312

] 1993

] Spectral Classification With the

.] International Ultraviolet Explorer:An Atlas of B-Type Spectra

i

-]

-]

-]- Janet Rountree and

] George SonnebornGoddard Space Flight Centerp

] Greenbelt, Maryland

1

]

]

.]

National Aeronautics andSpace Administration

Scientific and Technical- Information Branch

IMA

SA

The

1981C

onference

On

Rem

ote

Sen

sing

Ed

ucatio

nM

ay18-22,

1981S

ession

ST

AF

FN

EE

DS

FO

RE

FF

EC

TIV

ER

EM

OT

ESE

NS

ING

EX

PLO

RA

TIO

N

byJam

esR

.D

avisP

hillipsP

etroleumC

ompany

Bartlesville,

Oklahom

a

Rem

otesensing

isassum

inga

role

inthe

searchfo

rnatural

resources.R

esearchhas

shown

thatsatellite

imagery

may

beim

portantin

locatingcertain

typesof

petroleumand

mineral

deposits.

Either

director

indirectindications

ofnatural

resourceoccurrences

haveto

bedetectibl,

fromstandard

orenhanced

imagery

data.T

heseindications

arethe

resultof

geochemical

alterationof

_oilsor

geochemical

stresson

vegetationin

affectedareas

ascom

paredto

thesurrounding

unaffectedarea.

Traditional

mapping

ofgeological

structurecan

beaccom

plishedusing

satelliteim

agerydata.

Inpetroleum

explorationthis

may

behelpful

inrem

oteunderdeveloped

countries,but

probablyw

illnot

beutilized

extensivelyin

well

mapped

areassuch

asthe

U.

S.,

Canada,

andE

urope.

Inthe

caseof

petroleum,

itis

generallyaccepted

thatpetroleum

migrates

tothe

surfacew

hereit

caninteract

geochemically

andgeobotanically.

Petroleum

rangingfrom

asphaltto

methane

isencountered

asseeps

orm

icroseepsin

soilsabove

petroleumtrapped

atdepth.

To

nalano

malies

have

beenrepo

rtedo

nLandsat

imagery,

for

example,

fromW

yom

ing.It

isbelieved

thatiron

depletionand

thepresence

ofhydrocarbons

inthe

soilover

theP

atrickD

rawfield

may

bethe

causeof

thestressed

sagebrushat

thatlocation

(N.

L.F

roman,

1976and

R.

W.

Marrs

andR

.G

aylord,1981).

At

otherlocations

suchanom

alieshave

beenattributed

todevelopm

entroads

andw

elllocations

developedafter

thediscovery

ofan

oilfield.

Tonal

anomalies

inRailroad

Valley,

Nevada

providean

interestingcase

forthe

useof

enhancedim

ageryto

clarifyan

anomaly.

Oil

was

discoveredin

theE

oceneat

4000feet

belowthe

valleyfloor.

The

anomalies

donot

coincidew

iththe

outlineof

theknow

nproduction.

This

casew

ouldprovide

agood

caseto

investigateboth

geochemically

andgeobotanically.

34

] SPECTRAL CLASSIFICATION WITH

1 THE INTERNATIONAL ULTRAVIOLET EXPLORER:AN ATLAS OF B-TYPE SPECTRA

] by

Janet Rountreoand George SonnebomLaboratory for Astronomy and Solar Physics

] NASA/Goddard Space Flight Center

1I. Introduction pose without reobserving the standard stars to make sure that there are no system-

A set of criteria for the spectral classification of B stars in the ultraviolet atie effects.was published by Rountree & Sonneborn (1991, Paper I). In that paper it wasshown that photospheric absorption lines in the 12(K)--1900A wavelength region II. Data Processing

can be used to classify the spectra of B-type dwarfs, subgiants, and giants on a The spectra comprising this Atlas were taken with the IUE short-two-dimensionalsystem consistent with the optical MK system. The stellar wind wavelength prime (SWP) spectrograph in the high-dispersion mode. The ex-lines are not used for classification on this system. Stars with peculiar wind lines traeted spectral data, produced by the standard processing provided by the IUE

are distinguished from "normal" stars, and are marked with the suffix "w." The Project, were resampled to a resolution of 0.25A, normalized to a rough eontin-observational material used in Paper I consisted of high-resolution spectra from uum level between 1150---1900A, and plotted on llin. x 17in. paper on a laserthe International Ultraviolet Explorer (IUE) archives, suitably resampled and dis- printer. For details of the data reduction steps, see Walborn, Niehols-Bohlin, &played. Insofar as possible, the standard stars on which the ultraviolet elassifiea- Panek (1985) and Paper I. Our data processing procedures differ from those of thetion was based were chosen from among the MK standards, previous authors only in that the continuum normalization has been made autono-

] A numberof representative spectra were shown in Paper I, in order to il- mous rather than interactive and that the plots were produced on a laser printerlustrate the classification method. But these spectral plots were reduced in scale rather than a CalComp plotter. The software needed to resample and normalize

] by approximately 50%, and thus were not suitable for practical classification the spectra is available at the IUE Regional Data Analysis Facility at Goddardwork. The purpose of the present Atlas is to make available a larger number of Space Flight Center. If the user does not have access to a laser printer that aeeom-

spectra at the scale used for classification. These spectra represent a densematrix modates 1lin. x 17in. paper, the spectral plots may be produced piecemeal on• of standard stars, and also some interesting individual eases. Readers may use the smaller paper, but the original scale (10A/em) should be preserved. It is stronglyrecommended that any spectra last processed before the improved extraction soft-figures in this Atlas to classify their own IUE spectra, after processing the data as

L] described in Section II below. The recommended procedure for spectral elassifi- ware was put into production (1981 November) be reproeessed by the IUE Projectcation with the Atlas is described in Section IV. before undertaking the resampling procedure.

] Although the Atlas shouldbe useful as a guideline for ultraviolet spectralclassification with instruments other than 1UE,it should not be used for this pur-

l

]

2

Ia) whose spectra appear here are the stars described by Walbom & Nichols-III. Description of the Atlas Bohlin (1987). These stars have not been classified on the ultraviolet system m

All the stars whose spectra are presented in this Atlas were drawn from the spectral types given are the optical MK types. The supergiant spectra are re-the list in Table 2 of Paper I or from a second list of approximately 100 stars that produced in this Atlas in order to show the full range of variation of certain spee-were subsequently classified (without knowledge of their previous MK types) on tral lines as a function of stellar luminosity.the same ultraviolet system (Rountree & Sonnebom 1993, Paper II). In general, Part 2 of the Atlas, Plates 15---20, illustrates the effect of rapid stellar ro-these are stars with visual magnitudes brighter than about 6.5, having normal MK tation on the ultraviolet spectrum. Each plate in this section displays two pairs oftypes in the range B0---B8 III_V according to Rountree Lesh (1968), Hiltner, spectra, each pair, closely matched in spectral type, consists of the spectrum of aGarrison, & Sehild (1969), or Morgan & Keenan (1973). A few supergiants were slowly rotating star (v sin i usually <50 km/s) and the spectrum of a rapidly rotat-drawn from the work ofWalbom & Nichols-Bohlin (1987). ing star (v sin i usually >200 km/s). Although most of the rapid rotators are not

The spectra are arranged in montages of four or five per two-page spread, standards, these illustrations should be helpful to the user who wishes to classifyor "plate." The wavelength scale is indicated by tick marks at 10A intervals above the spectrum of a broad-lined program star, since they show how these spectra areand below each spectrum, with numerical values of the wavelength in Angstroms likely to differ from the narrow-lined standards.shown at the bottom of the page. The crosses along the wavelength scales mark Finally, spectra with anomalous stellar wind lines, primarily strong ab-the eehelle order splice points. The quantity plotted as a fine line at the top of sorption lines of C IV _,_1548, 1550, Si IV _.h1393, 1402, and/or N V _.1238,each spectrumis the normalized data quality factor, which in these plots primarily 1242, are illustrated in Part 3, Plates 21---26. These are stars whose ultravioletindicates (by a downward spike) areas in which the data points may be eontami- spectral types have a "w" suffix in the classification of Rountree & Sonnebornhated by a camera reseau. The most important spectral lines, especially those used (1991). As in Paper I, italics are used in the text accompanying Plates 21---26 toin classification, are identified along the top of each plate. The stars are identified distinguish ultraviolet spectral types from optical MK types. The spectrum of atto the left of their spectra. The spectraltype given for each star is the ultraviolet least one "normal" star of identical type is presented with each anomalous spee-spectral type; in most eases, this is identical with the optical MK type. In Parts 2 trum to show the good match in the photospheric absorption lines, which alone areand 3 of the Atlas the rotational velocity from Uesugi & Fukuda (1982) or the date used in classification. More detailed studies of some of these stars are referencedof observation is also given. Overall characteristics of the spectral type range coy- in the text opposite the spectrumin question.ered by each plate are described in the text at the left of the spectra.

There are three parts to the Atlas. Part 1, Plates lm14, contains se-quences of spectra of standard stars for direct use in classification. Plates 1---7 IV. Use of the Atlas

show spectral-subtype (or temperature type) sequences for dwarf (class V), After the user's program spectra have been processed as described insubgiant (class IV), and giant (class III) stars. Almost all of these stars are stan- Section II, they may be classified by direct comparison with the spectra in this At-dards listed by Morgan & Keenan (1973) or by Rountree Lesh (1968). On the las. As in the MK system, the ultraviolet classification system is defined by itsmain sequence, where very fine subdivisions are possible, we provide some over- standard stars, most of which are illustrated here. Therefore, a program starlap between the groups of spectra on successive pages, so that the user will always should be assigned the type of the standard star that it most closely resembles. Itbe able to bracket the spectrum to be classified between two standards. Plates 8_ must be emphasized that the comparison should be made using only photospheric14 present luminosity sequences at seven spectral subtypes. In these montages, absorption lines. The N V, Si IV, and C IV lines should not be used in classifiea-some of the standards in classes III_V have been replaced with other stars whose tion; they should be taken into account only in assigning the "w" suffix.spectra were judged to be equally representative of their type, so as to give asmany examples as possible of normal ultraviolet spectra. The supergiants (class

I

13

]Table 1 lists the standard stars of the ultraviolet classification system, as

I well as the photospheric lines used as classification criteria. This is a slightly up- Referencesdated version of the similar table in Paper I.

] In our experience, it is possible to assign a very accurate temperature type Grady, C.A., Bjorkman, K.S., & Snow, T.P. 1987, Ap.J. 320, 376.Hiltner, W.A., Garrison, R.F., & Sehild, R.E. 1969, Ap.J. 157, 313.to a star from its ultraviolet spectrum, while luminosity class may be more difficult Hirata, R., & Asada, Y. 1976,Pub. Astr. Soe. Japan 28, 713.

] to identify accurately (see Paper II). Therefore, we recommend first locating the Irvine, N.J. 1975, Ap.J. 196, 773.spectrum of a program star among the standards on the main sequence, and then Morgan, W.W., & Keenan, P.C. 1973,Ann. Rev. Astr. Ap. 11, 29.going to the luminosity-effects plate at that spectral type to see if the star appears Rountree Lesh, J. 1968, Ap.J.Supp. 17, 371.

] to be a subgiant or giant. If it does, its temperature type should be verified by lo- Rountree, J., & Sonnebom, G. 1991,Ap.J. 369, 515 (Paper I).eating the spectrum on the subgiant or giant sequence. Of course, this is an itera- Rountree, J., & Sonnebom, G. 1993, in preparation (Paper II).

] tive procedure, since temperature type and luminosity class are not completely in- Shore, S.N., & Brown, D.N. 1990, Ap.J. 365, 665.dependent. Finally, the N V, Si IV, and C IV lines, if present, should be compared Slettebak, A. 1982, Ap.J.Supp. 50, 55.with the same lines in the standard spectrum to see whether the program star has Sonneborn, G., Garhart, M.P., & Grady, C.A. 1987, in Physics of Be Stars, ed.

] an anomalous stellar wind. The behavior of the wind lines in the standard stars is A. Slettebak & T.P. Snow (Cambridge: Cambridge Univ. Press), 286.

described in the text accompanying the spectra in Part 1. It is also noted in italics Uesugi, A., & Fukuda, I. 1982, Revised Catalog of Stellar Rotational Velocities] in Table 1. (Kyoto: Kyoto Univ.).

Walbom, N.R., & Niehols-Bohlin, J. 1987,Pub. Astr. Soe. Pae. 99, 40.Walborn, N.R., Niehols-Bohlin, J., & Panek, J. 1985, 1-UEAtlasof O-Type

Spectrafrom 1200 to 1900A (NASA Ref. Pub. 1155).] V. Conclusion

i ] It is hoped that this Atlas will find extensive use in the classification ofIUE high-resolution spectra, especially for stars that have not been observed in the

] visible region. Spectral types obtained by the procedures outlined here and in Pa-per I should be entirely consistent with MK spectral types. In principle, the samestandards and criteria can be used for spectra obtained with a different ultravioletspectrograph, but in that ease the standards should be reobserved with the otherinstrument to avoid systematic effects.

I

I

1

[Table 1 - Ultraviolet Spectral ClassificationCriteriaand Standard Stars

4 I

V IV III V IV III [B0 u Ori HD 75821 HD 48434 B5 35 Eri, p Aur _ Her 5 Per, r Ori

1640A (He II) strong Interpolatebetween N III, N IV stronger Si II dominatesspectrum Si II, Si III, AI III Si II stronger thanB5 IV I1718A (N IV) strong V and III 1854-61A (AI III) stronger 1655A (C I), Fe II moderate strongerthan B5V1748-51 (N III) marked 1247A (C III) stronger 1670A (AI II),AI III strongSi IV, C IV strong absorption $i IV, C IV absorption N V, Si IV, C IV P Cyg profile Si IV marginal to absent Si IV present, C IV absent Si IV stronger, C IV absent

B0.5 HD 36960, h Lep 1 Cas B6 13Sex 19 Tau 17 TauN III present Interpolatebetween N IV, AI III stronger Similarto B5V butAI III Interpolatebetween Si II strongerHe II, N IV moderate to strong V and III N III present but weak stronger V and IIIC III strong Fe III weakerSi IV, C IV strong absorption $i IV, C IV absorption Si IV, C IV absorption Si IV absent Si IV, C IV absent Si IV, C IV absent

B1 toI Sco, 42 Ori QtVir o Per, o Sco B7 (xLeo 16 Tau qTauN IV weak to absent Interpolatebetween G III, He II, N IV stronger AI II, C I prominent Interpolatebetween Si II, AI II stronger

Si III 1300 multipletstronger AI III weakerthan B6 V V and III than B7V IHe II marked V and III

1247A (C III) strong Fe III absent|

1264A (Si II) presentSi IV strong, C IV wk. absorption Si IV, C IV absorption Si IV, C IV absorption B8 18 Tau No standardinprogram 27 Tau

Si II dominant Si II, AI II stronger

B1.5 HD 35299 h Sco 12 Lac AI II, C I prominent thanB8 V1264A markedbut <1247A Interpolatebetween Si Ul,C III stronger AI III, Fe III absentHe II weak V and III8i IV absorp., C IV wk. to absent 8i IV, C IV absorption $i IV, C IV stronger

B2 22 Sco ,/Peg it40ri1264A (Si II) = 1247A (C III) Si III, AI III, Fe III C III, AI III, Fe II, Fe III1310A (Si II) < 1300A (Si Ill) strongerthan B2 V strongerthan B2 IVHe II weak to absent 1600-10A (Fe II) stronger8i IV moderate, C IV absent 8i IV stronger, C IV absent $i IV stronger, C IV present

B2.5 o Sgr HD 32612 _r2Cyg1264A (Si II) • 1247A (C Ill) Interpolatebetween Si II, Si III, C III, Fe II, Fe III1310A (Si II) < 1300A (Si III) V and III AI III stronger1485A (Si II blend)present8i IV absorption 8i IV present, C IV absent $i IV strong, C IV present

B3 q UMa, q Aur HD 134687, 126 Tau HD 898901264A (Si II) >> 1247A (C III) Interpolatebetween Si II, Si III, C III, AI III,1310A (Si II) > 1300A (Si III) V and III Fe III stronger1485A (Si It blend)markedSi IV weak Si IV present, C IV absent $i IV stronger, C IV present

B4 HD 20809 53 Per No standardin program [1310A (Si II) > 1300A (Si III) Si II, Si III, AI III strongerthan1485A (Si II blend)prominent B4 V

Si IV weak to absent Si IV present, C IV absent t( m

15

'1

i!

1

1

!

1

i Part 1

.] Standard Stars

I

l

6Plate I a

Main Sequence Ol"_ Sil" IIIIIIIS=.1s=. [sii_m_vl' I ' I _ I ' I ' I _ I ' I ' I ' I ' I _ I ' I ' I ' I ' I

BO - B2

u Ori

B0 V

The earliest main-sequence Bstars are characterized by lines ofHe II h1640, N IV h1718, and N IT[hh1748,1751, which decreasesmoothly from B0 to B1. C IT[

h1247 begins to weaken at B1, HD 36960while the photospheric Si H lines;k1264and h1310 begin to increasein strength. The ratio _.1264/;k1247 B0.5 Vis approximately unity at B2 V.

In these standard main-sequence stars, Si IV ;kh1393, 1402 ,r--------_-----_r-------_ _----'----is mainly photospheric, and shows a _ ! V V [ [ 1marked decrease at B2. The stellar

wind lines C IV hh1548, 1550 are 42 Oriessentially absent by B2.

B1 V

v fHD 35299

B1.5 V

22 Sco l.

B2 V [

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 I

7Platelb

C IV HeII N IV N III AIIII Fe IIIH I I _ _ RI ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I '

J

--r V-]

•

1

]

I

II ...." : _-" ' ><1, x l 1× I ix I "" ,' --" ,' _<' I ×1 ,' :" I " _ '

_]I

, _ , I X ' I }(, I 'X I , _ ,

_.1 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

8

Plate 2a I

Sequence Cl'" s,i" ITITII-lS',,,s,,, Is,,__v] s,i"Main' I ' I ' I ; I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I 1

t

B2- B5I

22 Sco

The ratio Si II _.12641C m B2V _ _..V,__.1247increasesmonotonically from

¢

I

B2 to B5 on themain sequence,as "" ' "'- i "- ' ..[ >_ X i'- '" I "-' -_ "" I" ' "-i _- I "" ' "'i "" i "-' i'- ' "'I '" I "_ I ""does the ratio Si II _1310/S1 HI

h1300. The photospheric Si II linesh1485 and ;_1533 also become

a Sgrprominent in this spectral typerange.

B2.5 VSi IV ;_.1393, 1402 decreases

to marginal strength, while C IV_1548, 1550 is not normally pre-sent in main-sequence stars later

v vq UMa

B3 V

I

HD 20809 [. ,

B4 V [

35 Eri 1..

B5 V [.

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 [

9Plate 2b

] Si II Fe II C I AI II AI III Fe III

I--I _ I i I--I I-II ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I I I I I I I I I

] ,,

I

i

I _ I I I I I I _ I I I I II .. I , ... I , .. I v I _, I .,, ::IK IX IX I X I X I I X I XI I )( I ) IIxl x i ii A I I 1. I '^ I _" I "" I _"

I r-_ v

1

I,'×', ',-,,,: "_,_:'×,' ,A,'-" ' Ix ,' _ ,' _I '

I _ 7 y-v _--_ 'v_-V ,'y r---T

.!I><: ,..'--: ._-_'. ..,'-' ,..'-- ,' :>.-,' m ,' x I _k I

I --T--T+ ....I _'l--_ /-v , i_ T_I

I X I _( I ' X I ' k I , _( I , :J( ,-- 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

10 Plate3a.

.

MainSequenceB5- B8

The lines of Si H dominatethe Si II Si III Si II Si IIstellar spectrum throughoutthis ] ]Ill ]1 ] ]

types ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' Irange of main-sequenceFe IH X;_1892, 1896 weakens attypes later than B5, while A1 HI;_1854, 1861 /caches a maximum 35 Eriat B6. /_

B5V

I_Sex

B8 V

Leo / IB7V _ _X f_._.._-, v, v, _ _ _ ,v , _, ,v , v, ,v , v, ,v . v I^,..,^, .., .., _ _ _. ,..,.., _ _ ,.., .., x Ix, xl ,x I v' ' _/\ ' I/" ' /\ I _/x I _ I /x I18Tau l.

B8V I

_;, 1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 l.

1

• } Plate3b 11

1

1

1Si II FeII CI AIII AIIII FeIIII-1 _ I I Iml n

I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I '

! v _ ? v • _ ' I ' v _-T11

,,. = ,_ : _ =x' ,v, "" ' " ' "" I I I I I I I I ,v = ×I :× = ,_ =I ' " I "" I _" I _" _K X IX I X I X I )( I !: '

i ---m--'-_m-_• _ l '__ _ v'-V i q' 't i ,v ! v-T-i

A A /_

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1640 1860 1880 1900

12

Plate 4a ].

i Subgiants °1'" sll" III IIIIS',. s,. rs',____VlS_l"'' I ' I I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' 1

a0- B2 _ _ 1 _ _ _ _ I J _

BeH°"'",v ,lines. C IV XX1548, 1550 can X Lep I

sometimes be seen as late as B2.B0.5 IV

HD 63578 I

B1 IV Xx x _=xl x= x _, ',xl = q x I'-'= xl x I"-= "_ =x I x= 'x = --' ,--'i -',l '-', i X I >( '

_ v 1 r---T--y v----__ _ i ,-I ] , -w- i

,..,.., .., ..l -4 ::< _< _><, .. v-.. , --. .- Ix='< x I;<_ --,'" ,v ,.., "" _>< l.1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 •

113

Plate 4b

C IV He II N IV N III AI III Fe III

FI I I I-II I--q I-II ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ° i ' I ' I ' I ' I ' I ' I ' I '

i

] I><I i xl I• _ I "" I I I

1

I

1

1

I

I

I , I I X I" 1500 1520 1540 1560 1580 1600 1620 1540 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

14Plate 5a

•_ _'_'_°u_"_"an*s c,,, s,,, s,,,,s,,, s,,v s,,,, s,,,I I VITI-1VI I--] I I' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I

B2.5- B7 "V _ V "HD 32612

B2.5 IV

The photospheric Si IV linespersist until type B5 in thesubgiants. The relative strength of

the Si H and Si lII spectra makes a [ _- _ Vuseful spectraltypecriterion.

126 Tau

B3 IV

-r Her

B5 IV

19 Tau

B6 IV

16 Tau [

B7 IV

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 ""

15Plate5b

Si II Fe II C I AI II AI III Fe III

f-I f-A] I I I--] nI ' i ' I ' I ' I ' i ' I ' I ' i ' I ' i ' i ' i ' i ' I ' I ' i ' i ' I ' I '

1

1

1

]

]

I

-]

1

_( I _( I "X I × I _< I TX I I X I I XI , _ I I )( I I Xt I I X I I )l_ I1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

16 Plate 6a

Giants N_V CI III Sil II _-[-_--_SIIII SI II [--ISiIV' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I

B0- B2

HD 48434 [

In the giant stars He II _1640 BO IIIpersists to B2, N IV X1718 to B1,and N 111XX1748, 1751 to B0.5.Although C HI X1247 is stronger "" ' "" , -'" ' "", -*',' -'_ -", v'" '-'" , "" ' "'1 "" , _" ' "", "_ , -'" ' "'t '-'" I -"-' v'" ' -'", '-'" , ,'_ , -",than on the main sequence, the ratioM264/;_1247 is stiU near unity atB2 HI. Si IV hX1393, 1402 andC IV XX1548,1550 exhibit P Cygni 1 Gasprofiles at B0 HI, and remain asstrong absorption lines throughout BO.5 Illthis spectral type range.

[a Sco

B1 III

12 Lao { o

B1.5 III

B2 Ill I......

1200 1220 1240 1260 1280 1800 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 [....

1

]

1

1

.]1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

HD 89890

B3 III

Si IV persists to B5 and C IVto B3 in normal giant stars, but thespectrum of stars in the B3_B8range is still dominated by Si IIlines.

8 Per

B5 III

17 Tau

B6 III

q Tau

B7 III

27 Tau

B8 III

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 [

19Plate 7b

] Si II C IV Fe II C I AI II AI III

I--1 17 F--TF1 I I 7-1I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I '

1

] I><' I_ ' _ ,.v,_, .,v,_. , ,_.,v ,' =_ I _ I b< ,, ,../,A , =v,_-, = _ ' I_ I t><' I J_ I ' _1 '

11

! I_' I_ : _"_ : _,v, ,_-,,v , Ix I _@'

,,_,,VV• -,l

II><' Ix ' ><I,,v,A,,,-,'A, ,'v,_, _ ',_K I _<' I ><'I t>{ J

Il

'-- '_ -_ :,<' ,,,' Ix ' "-' "" ' _ ' "" I _< ' ""' ,v, : xl l _< z IxJ I xl ' '"' : "_ :I "" _ i" I "i I ' "" I I _" I '_ I I "" I ''" I ' "" I I ' _" I ,i,

] --r--- i -,v ...._r _ 'q 't l _ _i _-v]J

, )I< , IX ' I Xl I 'X I ' )I: I

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1640 1860 1880 1900

2OPlate8a

LuminosityEffectsat BO

[

The indicatedlines of C m, NV C III Si IVN IV, N m, and AI m an mc_ase V] I [--]A.in going up the luminosity sequence I ' i ' i ' i ' i ' i ' I ' i ' i ' I I_ ' i ' i ' i ' = , ifrom main sequence to giants. The " :_ .......i'-" ' -" ; .............. _......wind lines of N V, Si IV, and C IV I

exhibit P Cygni profiles in giants 60riand supergiants.

BOla

" '",.-,' -,_ :X _' X= ,-,Iv = vl,,, =X ', X I Xrr-..-.,_.---._

HD48434

BOIll

HD75821

BOIV

. I

v Ori {

BOV l" 1

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 I

21Plate8b

C IV He II N IV N III AI III

I7 I I 17 I--1I i I ' I i I ' I ' i I ' ' I i I = I ° I ' I i I ' I ' I , I i I ' I , I i

]1

,_l --rr-n- "

1I )( , Ix , XI , ). I , .." I ,.... I A"" I .."" I _ I .."" I .._" I 'X I , ..'" I , ..'"I , .1... , I ..'" , I ..'" I , ..'" I , ;_ ,

J 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

22 Plate9a

LuminosityEffectsat BO.5

_.o_m.._..m.... . .vc.., "'vl °i"'A1 111"lines are luminosityindic,a- I ' I ' I 'tors. The stellar wind lines are in _.._._.,_____

absorption, except in the supergi- Vants.

.oriBO.5la

v I v, "v! _ Iv , v I v , vl _ I v , vl "_" I v , vl ,v I v, Iv _ vl ,v I "vf I vI /\ ' /\ I /\' "3 _ V\ ' /\ I /\ ' /_1 _'\ I /\ ' '_,1 /\ I /\ ' "_ '/\ I /x, I/\ ' /\1 '/\ I "_ I /\

pCru

BO.5III

Lep

BO.5IV

HD36960 _BO.5V

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 l

23Plate 9b

]

1]

I X ' IX ' XI ' X I 'X I 'X I X I ), I ;_ I

] 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1640 1860 1880 1900

24 JPlatelOa

LuminosityEffects {at B1 [

JThe Si IT[multiplet at _.h1290- C III 8i III C 8i IV 8i III

1300 is luminosity-sensitive in the I _ I--I IB1JB3 spectral type range. C H, ' i ' t ' i ' i ' i ' i ' t ' t ' i ' i ' i ' i ' i ' t [Si IV, C IV, and A1 Ill exhibit P

Cygni profiles in supergiants, but /not in stars of luminosity class HD148688ITIJV.

B1la

o Per

B1III I

I

HD63578BI IV _,_ 1,.

v , v " '"''" xl I xl I Ix /\1 _/\ I /x I A

_-Y -_--_ l---F i r - 1to1Sco {

B1V l....

× I.1200 1220 1240 1260 1280 1300 1320 1340 1860 1380 1400 1420 1440 1460 1480 1500

25PlatelOb

1

1

.....

!

i

]:1

.. ,.. ._ =.., ,.. i ,v I _ I >_ I _ I >_ I _ I _< I I× I ix I J _q I Ix t I ×l I I× I I ×1 I

J

_._]

X I X I × I "X I _ I lX I i X I i XI i h i I X I I X i I IX I i _,_ ,1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

26 Plate1la

LuminosityEffects Jat B2 I

+] 27Plate1lb

1

1

1

1

l

!I I xl I I I I _1, I I'" I I ×' I I><l I H IX I X I I X i .. I ,.. I _.. I .i., I _ .,,.."" I n."" I .""I.... ,' ..I... i ..I'" I" 1...."" i '' I " I "" I I I i I

1 --r-F- v '--!--_ r ----P _1 v .v- I

1'" " "'_ ="' "' =× I x I × I >" I >4 , Ix , 1×= ' " ' i ×1 iI "" I I'" I q "" I , -', I I 1-,. I

....I '!l-' _ -V---mO-_ I "_--]p I _r-" '] y 'l'- T

..I

....

t X ' IX ' _ ' X I ,;( I 'X I X I :K I X I 3I( , IX ' I X' I 'X I , )_ ,1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

2o ]Plate12a

LuminosityEffects {at B2.5 [

Theprincipalluminosityindic.a- C III Si III CII Si IV Si III Si IItors at spectral type B2.5 remain the I _ n [ml I Ilines of C HI, Si IT[, Fe H, and ' I ._,..---,,...-.....,-,....-.-__'I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' IFe HI. The Si II blend at X1485 VV _ _ V _makes its first appearance at this

I " '

spectraltype. The supergiantwind HD92964features of C II, Si IV, C IV, andA1HI are weaker thanat B2.

B2.5la

Cyg

B2.5III I

HD32612

B2.5IV

XLib _ 1._B2.5V

.',-/ - "v N/ , \i I v , vl v I v , vl v I \I , ,,,/I ,v I v, Iv , \/I ,v I I

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

I 29Plate12b

• ]

]

-1

C IV Fe II He II AI III Fe III

H r-m I _ N"] I ' I ' I ' I ' I ' I ' I ' I ' I ; I ' I ' I ' I ' I , I ' I ' I ' I ' I ' I '

1

l --F--w -l

I I I I I I''" "-<" ><1 I .-"' ,..,.., ....,., _ , ... , ., , ..- ' ,.. ' _× ' ',x' = "--t ' × ' xz sx , × ,I ,-,, I I t X " i I I i "" I "" I .4, i "" i I I

I ] -_F--Pi y 7 1 v -T!

1I "" I I" " "'i I X I I I I I , ,_, I , v II ' "" I i-_ I v- I _" I I I

! I IT-P I -_r 'x'r--r- -v _ vr'- _',_ -v "V"r--"T-I

___l

I _< I 'X I ' X I , _ , IX ' I X' I IX I ' XI ,

_I 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

13O

Plate13a

LuminosityEffects Iat B3

Linesof C m, Si11I,Fe H, and C III SiIII C II SiIV SiIII Si IIFem remainluminosity-sensitive at I ITiT1 I1 I-II I Itype B3. but show less variation ' i ' i ' = i . t . t ' i J ' i . I ' I i ' I ' t . I

than at ear.= types. The most _ ............... :............. - "_' _ !...._ ...."i- ...... _ ..... V_--

pmmment wind .e;atu_rem B3 __l_v ! !,_ tl ! __ i t !, I/ f _

supergiants is (3IV ;kh1548, 1550. O2 CMa I

B3la I ' i

Iv v g I x,4 iv I v, Iv I v/" ' /" I /" ' /" I I /". , z'. I t., ,,,, "_1 '/" I z., i/-. 1 X ] iv I 'vf' '/" I ,,x I /\

a D 198820 _ _ I _ _ a _ _

B3111 _A,, ,A v I v, _ v Iv I , _ M I' I v , vl v I X I vl iv I v, Iv vl IX I 'vr I v/", ' /, I "\ ' /", I /" _ "_ "", K\ ' ,'\ I /,,, , A I r,,, I /\ _ /", I ,"", AI '/", I /,,, i/\ I ,"",I I ,"'_ I /\

HD134687 !

B3IV L = _ I

v I /" ' /"1 /"' /-_ X I _ v v I v I v'/" ' /\ /Xl 'Y" I "\' ''1 "" I"". = _ =x I x: Ix i xl ,x I × ,^_ r - _ _...._ _ _--r _ '_ '_-

_V I 'Vl _d/ I_ I V I v , _ x/ I V I X/I V I V I _l IV I _/I Iv I vl IV I I

........ , , , /x /x /x X X {1200 1220 1240 1260 1280 1800 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 •

1Plate 13b 31

]

1

1

-1

' X I ' X I 'X I _... I ..v I ,-,_" I .._" I _X I i)( I i X I , ..'" I i _4 , I X t I Xt I1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1640 1860 1880 1900

32 .. Plate14a

LuminosityEffects [at B5 J

[I

Lines of Si H, Si HI and _ Ill Si II Si III Si II C II Si IV Si IIare luminosityindicatorsforclasses I I-T_-_ H [_] I

pergian ' i ' i ' i ' i ' t , i ' i ' i ' i ' i ' i ' i ' i ' i ' iHI, IV, and V. In the su ts,the wind fines of C II, Si IV, C IV,and A1 HIare in absorption.

q CMa

B5 la

HD209419

B5III

I1

_-Herl

B5IV

1

.

pAur [,..

B5V [....

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 {.......

33Plate 14b

]

1

1

Si II C IV Fe II C I AI II AI III Fe III

I--I rl l-l-rl i i l--I F1I _ I ; I ; I ' I ; I I I ' I I _1 ; I ' I ' I I I ; I I I ; I ; I ' I ; I ' ;

11

o

, ..v I i )( I i _ i I X t I X I I t.... I

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1640 1860 1880 1900

l

1

[.....

l

I

35

1

1

1

1

1

!

} Part 2

. Effects of Stellar Rotation

i__]

36 Plate15a

RotationEffects [atBO.5

With the exceptionof Si IV and C III Si III Si IVcIV,,dlth_n_ Sl_ lin_sin I ITITI I_1

ph phed ' i ' t ' t ' I ' i , i ' i ' I ' I ' i ' I ' t ' i ' i ' ithese stars am otos c. Theyare broader and shallower in the --_ _- !_rapidrotatorsHD 135160 and 5 Sco

I = " "

than in the slow rotatorsHD 36960 ;kLepand 3. Lep. Both width and depthmust be taken into account in esti-matingthe strengthof these lines for B0.5 IVclassificationpurposes, v _nt =50km/s

5 Sco O

BO.3IVv dn l= 180 kmls

HD36960

BO.5Vv=in1=35 kmls

HD 3s16o [.BO.5V [v_ l= 180kmls

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 [.

37Plate 15b

1

1

..]

-]C IV He II N IV N III AI III

I I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I _ I ' I ' I ' I ' I ' I ' I '

1

t,, ,,4 I )f t, _ : ,-- : : v l><1:"',-, ,--'"', :× ', _'" ', _ I _< I 'X I I ,_(I I X I I )I( I IX ' I XI I i)( I I )_ I1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

38 Plate16a

RotationEffects

B1 - B1.5MainSequence

Unlike the photosphericand C III Si II SiIII Si II SiIVstellar wind lines, the Lqtetstellar I I ITITII-I I--]lines are unaffected by rotation. ' _ ' I I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I I

They are easily picked out in the _ _ 1 --I- '-_ _ _ "- -

stellar spectrao, rapidmtatorsHD I_ __1_' __/__ _ _____

I

X1526, have both stell_ ind inter- ' , ,stellarcomponents. B1V

v sin l= 25 km/s i/" ' /" I I " /'t _ K\ ' /" I /\ ' "t r\ II X I X I )( X = ,vl ,v I v, Iv vl iv I \,€ I v/_ I/,, I /"' I/" I /" I I/., I /'_ I /"

I'_'='_.l/_,.;. _ v _. ,v ,v, v, .. ,v,l_ :x ', x: ',x = ;", ,x I × Ix [I /\ ' /\ I /\' /' _\ K\ ' /\ I /\ ' /3 x\ I /\ ' /\1 "\ I /_' I

]1 X vl v I v vl ,v i v, iv vl ,v I ,,_ I v/\ ' /\ I I/\ ' /\ I /\ ' /3 r\ I /\1 "\ I [x [N I/\ I [_i I/\ ] /\1 '/\ I /x I /\

•

v _Tnl= 240 km/s

vl I1200 1220 1240 1260 1280 1800 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

]Plate16b 39

I

!

.]

I

I

_t Iv vI ._ I )t

..]

]I X ' IX , XI , )( I 'X I _)< , I ><_ I 'X I _ >_

_ .I 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

40 Plate17a

RotationEffects I

B1.5- B2 Giantsand Subgiants

I

JRotation effects tend to be less 0 III Si II Si III Si II Si IV

pronouncedfor stars abovethe main I I FFm_ 1--1 fsequence, but they can produce _ ' _ ' i ' i ' _ ' i i ' _ ' _ ' i ' I ' _ ' j ' i , I /

apparent differences in the signal-to- _ _ __ V 1 _ r_ T-W'--

noise ratio (S/N). Note that the in- _I t _ _!_ _ll!_[i_4_ _ _ _ f _ _1

strumentalS/Nisab°ut30f°raU (xPYX __ _ _ _

the digital plots in this Atlas. _ _ _ [

lit Iv lin i = 2Okm/s

X , I X I v I v, ,,..! ,v I _ I \1 i,, , ,,, ,,. ..., x _ =x I x= >4 r'.. x = >,.I x ,,, . ,, ,,, . ,,, ,,.. , ,.< , ,,

r ,_ v-r '-_--T_-I-T 7 _ J _ l

.o,oo o ,B1.5III

I,sin i = 220 kmls i lv I v, v Ix/ , v I v , vl v I v _ I vl Iv I I.. ,... _,, i Xi ,,, :xl .,,.. i.'-. ',". I Xi >4 X ,,, ' -,i .", iX , -'_ ,...'v,_,...,v' u-, " Xl ,'v,-.i ."<" __v

•v r _ r--r--r---7 _ _ _ r----p-- I

, ,B2IV I

I

v dn i = 40 kmls 1..

I v I vl v I v I vl v I v vl v I v, Iv II /'. /_ I l.\ I ix /"1 '_\ I ix I _ix I ix _ v/..I,._ _,, : iX I X IX

_ _ _ r _----r--r--7 v r- Vt"r _ q--- I

",l/ Iv _ v I v n \,'1 k/ I V _ ",./I v I ",./ , vl ,',,/ I Ix,, , I , k/ I I |"" "" -" X' "/ /x X X1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1_<60 1480 1500 [....

]

1 Plate17b 41

1

-]1

C IV AI III

I-i [--1I ' I ' I ' I ' I ' I ' I _ I ' I ' I ' I ' I ' I _ I ' I ' I ' I ' I ' I ' I '

.]

.] ,v ,v ._ ,, .., .v , I I I I ' ' ' ' I >4 i I I I I,.. : ,A : _ A, ._, .× x × _ × , • , _." , .':.-, ',x , _ x I xi z× K × ,

1''" I× "_ ,,, ,v, "" ' ' ' I× I I ×t I '× I ' ti ^ : [ q I ""l '^ I '" I X I × ' * I × I _ I _ I IX I zxl , fl I ×

J

.lI ,,, I _, i _, , ,_ I x I _<1 , _ I I><' I IX I J >{ I

I

_ ]

' X I ix I X I X I ::K I X I X I Ix I ' X I ' XI , )1¢ I I X i I )(I I ,)( I n ),_ w- 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

_

42 Plate18a

RotationEffects {

B2.5- B3Subgiants

ILinebroadeningcanposea less C III Si II Si III Si II SiIV '

severe problem for the classification I I H-[-fl [--II I I

of the mid-B stars,where the stellar I I ' t t ' t ' t ' t ' i ' ' t ' I ' t ' t ' i ' t

wind is weak and the photospheric _ _ i _ [

Si II lines arenot yet saturated.For

example, HD 150745, with a v sin i _ Or[ Bof 285 kin/s, is one of the fastest ro-tators in this program,yet its spec- .i_trum is quite comparableto thatof B2.5 IVthe moderaterotator50ri B. v_ l =35km/s

I v , V I V, _, V I'_ I V V I _,_ _ I V , vl V I V , vl ,V I V, Iv I vl IV I _4 I v/\ ' /\ I /\ ' /\ I /\l f "_ t_ ' /\ /\ ' /_1 r\ I /\ ' /\1 "\ I /\ ' /N '/\ I /\= I/\ ' /\1 '/\ I /_ I /\

HD150745

B2.5IV Ivdn l= 285 km/s

HD184687B31V_ ____l _ _ _v Iin i = 40 ImVs

v v Iv , v v , x,.'l !./ I v , vl v I X I _ ,v I v, Iv , vl ,v I .vl I v/x , /\ I /\ _ /\ I Ix, /' _\ F'\ , /x /\ ' r'i Y\ I /\ ' /Xl "\ I ,Ix I /xo I/\ ' /\1 '/\ I /'_ I /x

"rTau i....

B3IV IIvsin l= 180 km/s

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

143

Plate 18b

1

]AI III Fe III

I--1 F1I ' I ' I ' I ' I ' I' _ I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I '

1

l

.]_ .. i.. .._ ,.. i ,,, k ,, _ .. ,.. "" I Ix I x : : -.- : x: :x : ._ '.I "_" [ i_, I I X I I I I i I I ,.I ,I, I I I I ,;

I "",4%"I I ' "" I ' "" I I I I I _" I '"" I "[" I I I I

1 _ _ _ y,lI

Ji

I 'X I ,>_ , Ix ' I X' I ,><I ,- 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

.°

44 Plate19a

RotationEffects !

B5 - B6 GiantsandSubgiants I

The spectrumof the late B stars Si II $i III 8i II Si IIis dominatedby lines of Si H, whose [ _ _ [

trength prin ipal ' J ' I ' I ' I ' ' I ' I ' I ' I ' I ' I ' J ' I ' I ' Irelative s is the c

the lines are accurately taken into T Oriaccount, it is useful to have bothbroad-lined and narrow- lined stan-dardspectra. B5 III

I _. r _ _t4.,€ IN_ IV _ _V_ V_ IV , vl V Iv , Vt ,V I V, IV , V' ,V ' X._ IV/\ ' /\ I /\ _ /\ I /\l / "_\ K\ I /\ ' /'t _'\ I /\ ' /\1 "\ I /\ ' "'4 '/\ I /\_ I/\ ' /\1 '/\ I /'_ I /\i

- -v-v-oCas

B5IIIvsin1= 255km/s

2 Lac

B6 IVvdn i= 60km/s

I

23Tau I....B6IVvdn l =285km/s l.

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 l....

45Plate19b

]

]

1

Si II Fe II C I AI II AI III Fe III[--1 I-1._. n r-m i

I I ; I ; I ' I ' I ' I ' I ' I ' I ; I ' I ' I ' I ; I ' I ' I ' I ' I ' I ' I '

1

i

1

1

i

1

I

..]._1 , v I , .. I ,v I _. I _ I I I I i X I I X I I I ' ;I I I )( I I II )( , I)( , . ....... .... X )( 7( X ( )(i

__.] 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

H

46 Plate20a

RotationEffects IB6- B7Giants

Many of the ]ateB giantstart- Si II SiIII SiII Si IIdards, including16 Tau, 17 Tau, I ITI-I-11-1 I

' I ' I ' I ' I ' I ' .I ' I ' I ' I ' I ' I ' I ' I ' I ' Iandq Tau,aremembersofthePle-iadescluster.Thisclusteris a par- Y---'-ticularlygoodsourceof broad-linedstandards, although nan'ow-lined_Drastarsarefoundtherealso.

B6 III ivdn 1=30 km/s

1

.

17Tau

B6 IIIvdn 1=215kmls I

I

I

20 Tau ]

B7 IIIvdn l =45 kmls [

v I,1Tau ,_ [....

' IB7 III [....vdn l= 210knds

l...1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

1Plate20b 47

]

]

]

I

I_q-r-_ ....._ l-v __I

-]

I><l ix I I>_ I >_ I >{ I _ I _< I

I IX I X I X I X I b( I I)( I I X I i XI I _ I I X I I Xs I i X I I )_ I1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

I

I

!

!

I

I

l

l .

49

1

1

1

1

1

1

1 Part 3

Stellar Wind Effects1

I50 Plate 21a I

Stellar Wind Effects .v c,,, s,,,, s,,v lN I r--1' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I "[

at B0- B0.5 [1

Both v Or/and T Sco are MK B0 V ' ,,A ,-,/ I v, I....standards for type BOV. In the ul- ,, I ,,_ I v [traviolet, however, a" Sco exhibits ".. , A i -- ' "- J "-. " -I"- r x ,'- t /x, ._ _. i ". , ".i _. i ".. "_ ,A i A, i'. I v i _ "_ i Agreatly enhanced lines of N V, _ _ _ _ V l _ _ _ ! _ v l_-

cation at B0 V, while "t"Sco is des/g--rSco _ _I____V__nated BO Vw, indicating that thestellar wind lines appear to be "ab- B0 Vw _ tnormal" in comparison with the r-standard. The two spectra of "rSco [/ v "..A I vl ,\." I v, Iv v I , v I ".-I I vpresented here were taken over three "x , "x I .-x , "x I /x, /3 ._x Kx , "x I "x , "'1 Y" I /x , /x I "" I "x , "1 ' "" I ""' i'x l A I ' "\ I "_ I .-x

years apart; there is no indication of _ _ _ _ _ __---__

long-term variability in the stellar ___v 't l,,_ __v_lI'.4_1 _'__

wind, but variations on a shorter I___ _Itime scale cannot be ruled out. a" Sco

Walbom, Nichols-Bohlin, & Panek , ,(1985) also describe the enhanced B0 Vw ^stellar wind features of "r Sco,which they classify as B0.2 V. laa7Aug 18 "../I v I ".1t Tv I '../i I\/ \/I . v I

f I -,-il IX/ I "..i I V , ",.A 't../ I v I ix I -,./ l /_'1 I/x i ix I /_ I )(Although it is a 13Cephei vari- /'. ' /" I /" ' A I /"' /3 A-.. Ii\ ' /" I .-x , "'I Y" I /" A I /" '/" I A, '/" I

Bo.5Violetspectrum. In contrast,HDgiven53974,type of B0.5 £II and a normalultra-B0.5lllwllltheWh°Se(R°untreeultravi°letby RountreeOpticalLeShclassification&type1968)'SonnebomiSalSOwasofB013Cru.5III !_ __ 4_ }___' I _ __ _ I_____ 11/_ __ _ _t!_ _!_,! _l_(1991), who cited its broad stellar j i.., , ....1 )( i b( I v ) i I_(wind fines and especially the P ,-x ,,-\ I >1 I v lI )/', /A X b( IT i X l >_ b(i IV I X IX

B0.5 IIIw __, x., I X I v , xA _... I ../ , vl "*/ I \/ , ..A ,x/ I ",tv Ix/ , \!1 ,v I X I )/

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

51Plate21b

]

1I × I I.-'": ..,-" : --'., ,'--..,' ."-..,' x I "<1 , :)14 , I >< , I XI I 'X I , :_ ,1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

.

52Plate 22a

Stellar Wind Effects Nv o,,, s,,,, S,,vI7 I ITm [--II ' I ' I ' I ' I ' I ' I ' I ' 1 ' I ' I ' I ' I ' I ' I

atB1 _ v V I _ _ _ 1 - V'--V_ I __ 17_'l__-

oPer _.._... (_, _/__V_ _n___ ___

B1 III L,_

The MK standard for B1 111is I

oPer;aScoisa[_Cepheivariable , ._ v, ._ v I v ,, vl v I .. ,, )_ IX I v, Iv \_1 ,v I \. I v/'_ I /', I /_ I /_ I /" ' ''1 "I" I"" ' "" I "" ' /'1 "" I /", /", I "" I /" I /", ' I/', [ /", I ' "" ''_ ""and a spectroscopic binary, but at I I

-ntical and its ultraviolet spectra are __?__i

_jlC'lVla,another 13Cephei variable,is classified B1 IIIw because of the , 'P Cygni profiles of the N V and B1 IIIwC IV lines, and the weakness of the I

Si IV absorption lines. Rountree I ,1, ..._and Sonnebom (1991) cite evidence X '...i X : >.-.I "-' -"1 X rk<. , "- I -'- ' "'1 "- t ><1 ,.-< ] Xl IX t ><I .'v.-. II """ II .-.'"

for a variable stellar wind in this "V" i -__r__T_._............. _ _ _! _ I

(1987)star'Grady'describeBj°rkrnan'2VulasandaBeSn°WstarcrSeo .d]__ _'_ _____ _q_Y ___;i _@____'with a variable wind and a partially

resolved discreteabsorptioncompo-BIlII _ /'i'i 1' ! 'Ill V /nent. In the exampledisplayedhere,

the CIV doublet is greatlyenhanced . v..l [ X IX I

trumincompariSOnofHD63578.with"theThenOrmallatterstarSpeC-is "" ' "" I "" : X [ X l >J _ _ ',X X ', )_ ._< X I X _->_ IX 1 X', iX ', X I ',X i _ [ X

arapidrotator(vsini=2OOkmls). BIHDIv63578_ ,p_ __ q___/_/I/1, /___ _d__/_

..,..,.., x l Xl )K IX:Ix Ix, .-a -"" I-'- ' --1 "" I". ' "'t "" I xi Ix , .., ,.. , .. ,..v-v I Y

...., xA ._/ , \/ I v , vl ._.- I ...- , ,vIv I i X' iv . ><l ,>< t X /1200 1220 1240 1260 1280 1300 1820 1840 1360 1380 14,)0 1420 1440 1460 1480 1500 L_

1

!1

1

1

-]

1

.1

_X I X I X I _( I _ I 'X I ' X I , )(I , )I( , IX '- 1500 1520 1540 1560 1580 1600 1620 1540 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

54Plate23a

Stellar Wind Effects c,,, si,, , s,,,,sJ,, si,vI I IIIIII I r_l' I ' I ' I ' i ' I ' I ' I ' I ' I ' I ' I ' I ' I ' i ' I

at B1.5 - _---- _

HD 70930

B1.5 III

HD 85871 and HD 166596

have anomalously strong (3IV lines,in comparison with the normalB1.5 III spectrum of HD 70930.The Si IV lines have peculiar pro- I

files, in addition to enhanced line HD 85671I

strength.

The C IV lines, normally absent B1.5 IIIwat B1.5 V, are prominent in the spec-trum of 19 Mon. Grady, Bjorkman,& Snow (1987) describe this star ashaving a variable stellar wind.Emission at Ha is cited by Irvine [(1975) and Hiram & Asada (1976). I

HD 166596 vV_

B1.5 IIIw

HD 35299

B1.5 V

19 Mon I_l [.

i v, , X _ ,v i v, ,.A .,.,. i v , v1 v iv , .,_ 'X t I ,.,.I 'X i X _ v\ /\ /,, /x ,", /', /-, /\ /-, /\ _-\ /\ X t )( n /\ /\

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480- 1500

i

]

]V r_

1

] v, ,v , =x I _ I _ I _ I :_<t _< t 1><, I x, I 1>f ,Ixl × , _ :^, ,A,

11

I

I I _( I ,>< I ' XI , )I( , IX ' I X' I 'X I , )_ ,1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

56

Plate 24a IStellar Wind Effects o,,, s,,, s,,,,s,,, s,,vI i ITml-I f--]

I I

I I ' I ' I ' I ' I ' I I ' I I ' i ' I ' I ' I ' i

B2 Dwarfs _ _ I ' 1 _

a2v /_ ; J

The ultraviolet spectrum of >_ t13 Sco is normal for a rapidly rotat- X j v : ._i v, ...4 .._ k.. v [ _... I v ] I v : .d.`1 ,v m v, iv vf ,v i [ing B2 V star (vsin i= 225 km/s). "" "" i -'- .... - v"- ', .-. X I >_ "" i -- " X )< i "'. '' i -'.' i'" " "-i '' i _ X

In particular, the C IV lines are van- _ I _---- _ _ _ _ishingly weak. The other B2 dwarfs

depicted here exhibit different de-HD37017 fl_V_/_t__I_1__ _l_t___

grees of C IV enhancement. The

choppiness of the spectra of HD _/_57150 and HD 161056, due to a B2 Vw

?/Lpoor echelle tipple correction in thedata processing, makes precise clas-sification difficult. "" I "- ' ""1 X l >< X _ : X II ,..Iv -'1,,4 ,-..v I'"lv I X[ _4 IX [ X l I><t [ X

Shore & Brown (1990) reported _ vw _----__ _ _C IV and Si IV line variations in HD

37017. Balmer line emission in HD 57150 _MLJHD 57150 and HD 72067 has been

described by Slettebak (1982). B2 Vw: _A/ " l_ / [×' '_'l ><',><1><' >< x I><,x ><' >4 ><' ><l _<' >4 '><1 Ix , ><l '>" Ix

B2 Vw _/

' " x l x Ix _ "" ' "' "" xl _x I >4 I x-..-.. ><_xl ><t ><_x Ix _>< ><_xl _< ,--', x! ,....., ,..

f ,/ '1200 1220 1240 1260 1280 1:300 1:320 1:340 1:360 1:380 1400 1420 1440 1460 1480 1500 t....

1

!! _ __v-_- 'v -_--q I...._ ] '1

] I x , I× ' _1 ' ×I ,x I '× I __ I _ I D_ _ I× , I×' I ,x I I ×l ,

1 _--fl--- i -_ fl ' l " T--_-v 1_, v-

] I× , x , >(_ Ix I '>_ I >_ I >(I , h , I )< , I ×, I ,× I , >_ ,

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

58Plate 25a

Stellar Wind Effects Nvc,,, s,,, s,,,,s,,, s,,v lI-1 I I ITml--1 I_1' I ' I ' I ' I ' I ' I ° I ' I ' I ' I ' I ' I ' I ' I

The B2 Subgiant _ Cas

Cet

B2 IV

The 13Cephei variable/5 Cet hasa normal ultraviolet spectrum for aB2 V slow rotator (v sin i = 10km/s). The N V lines are absent,Si IV lines are moderately strong, [

andC IV is very weak. In_ Cas, _Cas1

which is not a 13Cephei variable, thewind lines are all enhanced and are [variable in strength. This variation B2 IVw I

is especially remarkable in the C IVlines. Sonnebom, Garhart, and lee2S°p7 [Grady (1987) set an upper limit of

l

several months for the time scale ofthe wind variability in this star. I

HD 163472 (B2 IVw) has an _ Casultraviolet spectrum very similar to I

Cas. Its potential variability has [notbeenstudied. B2 IVw

1982 Nov 261t

I

Cas {B2 IVw

/1983 Oot 2[

B2 lVw 1....19_4 Feb 12

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 [

} 59Plate25b

C IV AI III

I-1 I--1I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' I ' ' ' I ' I ' I ' I ' I ' I ' I ' /

i _ . , , , -_] .,-i_-___-m_- ' - r?-,_ -] V_ V-,] _-t. V ,..3-1]

]

1_v P I -] t--T I-

f

i

!

!'-- '-- ' =x { '×l ,xl , $ , Ix, I ×' l '× l ' >1 '

.1

I "" I t" I q I X I I I I I I II ' "" I '' I _ I "_" I :::K "" I "" I "" I ' "" I ', X I I X I Xl I )( I I

j I X ' lX , y,4 , >< l 'X l ,>,( I I X I l ,_ { IX I I X' I 'X I , )_ ,• 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

..

60 Plate26a

StellarWindEffects IMid-BDwarfs {

HD 192685 is essentially iden- C III Si II Si III Si II Si IVtieal with the B2.5 V standard ] I fflqql--1 I--1er Sgr, except for the abnormal ' J ' _ ' _ ' I ' _ ' _ ' _ ' _ ' I ' _ ' u ' I ' _ ' I 'profiles of the Si IV lines and theabnormal strength of the C IVdoublet. In I-ID72356, all the stellar o"Sgrwind lines are enhenced in compari-son with the B4 V standard HD20809. B2.5V

HD 192685

B2.5Vw J

1

I

HD20809 lB4V

l

[HD72356 l..

B4Vw 1I "v_ I

/N !

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500 I..

61Plate 26b

1

/

-.]

..]C IV C I AI II AI III

I-I I I I--1"] I ' I ' I i I ' I i I ' I ' I ' I ' I ' I ' I i I i I i I ' I ' I ' I ' I ' I i

}1

} , .. ,.. ._ v, '" ' :x ' _<1 ' _ ' I x , I xI I Ix I 1 >f 'I "" : I'" : "'t I " I ' "" I I

1

!

' X I iX I b< I , X I i._ 1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

Form Approved tREPORT DOCUMENTATION PAGE OMBNo.0704-0188Public reportingburden for this collection of information Is estimated to average 1 hour per response, includingthe time for reviewing instructions,searching existing data sources,gathering and maintaining the data needed, and completing and reviewing the conection of information. Send comments regarding thisburden estimate or any other aspect of this [collection of information, includingsuggestionsfor reducingthis burden, to Washington Headquarters Services, Directorate for Information Operations and Reports. 1215 Jefferson IDavis Highway, Suite 1204, Arlington, VA 22202-4302, and to the Office of Management and Budget, Paperwork ReductionProject (0704-0188), Washington, DC 20503.

1. AGENCY USE ONLY (Leave blank) 2. REPORTDATE 3. REPORT TYPE AND DATESCOVERED

Au[_ust1993 ReferencePublication I4. TITLE AND SUBTITLE 5. FUNDING NUMBERS

SpectralClassificationWiththeInternationalUltravioletExplorer:AnAtlasofB-TypeSpeclra

6.AUTHOR(S) 680 [/

Janet Rountree and George Sonnebom I7. PERFORMING ORGANIZATION NAME(S) AND ADDRESS (ES) 8. PEFORMING ORGANIZATION

REPORT NUMBER

GoddardSpaceFlightCenterGreenbelt,Maryland20771 93B00096

9. SPONSORING ! MONITORINGADGENCY NAME(S)AND ADDRESS (ES) 10. SPONSORING / MONITORINGADGENCY REPORT NUMBER

NationalAeronauticsand SpaceAdministration I

Washington,DC 20546-0001 NASA RP-1312 [

11. SUPPLEMENTARY NOTES

Rountree and Sonneborn: Goddard Space Flight Center, Greenbelt, Maryland 20771

12a. DISTRIBUTION l AVAILABILITY STATMENT 12b, DISTRIBUTIONCODE

Unclassified - Unlimited

Subject Category 90

13.ABSTRACT (Maximum 200 words)

Newcriteriaforthespectralclassificationof B starsin theultravioletshowthatphotosphericabsorptionlinesin the1200-1900Awavelengthregioncanbe usedto classifythespectraof B-typedwarfs,subgiants,and giantson a two-dimensionalsystemconsistentwiththeopticalMK system.Thisatlasillustratesa largenumberof suchspectraatthescaleusedforclassification.Thesespectraprovidea densematrixof standardstars,andalsoshowtheeffectsofrapidstellarrotationand stellarwindson thespectraand theirclassification.Theobservationalmaterialconsistsof [

high-dispersionspectrafromtheInternationalUltravioletExplorerarchives,resampledto a resolutionof0.25A, [uniformlynormalized,andplottedat 10A/crn.Theatlasdisplayssuchspectraforabout100stars,arrangedinspectral-type,luminosity,androtationalvelocitysequences.Theatlasshouldbe usefulfortheclassificationofother iIUEhigh-dispersionspectra,especiallyforstarsthathavenot beenobservedin theoptical. [

1!

14. SUBJECT TERMS 15.NUMBEROF PAGES It65

IUE;B-typestars;stellarclassification;stellarrotation;stellarwinds 18.PRICECODE!

17. SECURITYCLASSIFICATION 18. SECURITYCLASSIFICATION 19. SECURITYCLASSIFICATION 20.UMITATION OFABSTRACT [OF REPORT OF THISPAGE OF ABSTRACT

•Unclassified Unclassified Unclassified UL !

NSN 7540-01-280-5500 Standard Form 298 (Rev. 2-89) IPrescribed by ANSI Std. Z39.18 t298-102

....

,]

L

I

I

!

J

..J

.... i

_.1

Na,onaicsanOSpaceAdministration SPECIALFOURTH-CLASSRATE 3 1176 01404 6131

POSTAGE&FEESPAID [Goddard SpaceFlight Center NASAGreenbelt,Maryland20771 PERMITNo.G27

OfficialBusiness I--Penaltyfor PrivateUse,$300

$4 001 RP-1312 930722 S017690 A [-NASALANGLEY RESEARCH CENTER

ATTN : SUSAN ADKINS, HEAD REF SERV SEC [TECHNICAL LIBRARY, MS 185HAMPTON VA 23681000I

[

IPOSTMASTER: If Undeliverable(Section158,

PostalManual)DoNotReturn

i................ , Idbnrnnhlln I II1 ....................... ii -iiiiii --i_Ti1 I II ...................................................................................

•

I

I

I

[

J_

.

.

L_

t • L

! FoP.l Nc · 2020. 3. 17. · the same ultraviolet system (Rountree & Sonnebom 1993, Paper II). In...

Documents

Transcript of ! FoP.l Nc · 2020. 3. 17. · the same ultraviolet system (Rountree & Sonnebom 1993, Paper II). In...