An HI interstellar bubble surrounding WR85 and RCW118
a r X i v :a s t r o -p h /0507481v 1 20 J u l 2005
Mon.Not.R.Astron.Soc.000,1–??(2002)Printed 5February 2008
(MN L A T E X style ?le v2.2)
An H i interstellar bubble surrounding WR 85and
RCW 118
J.Vasquez 1?,C.Cappa 1,2?and N.M.McClure-Gri?ths 3
1
Instituto Argentino de Radioastronom′?a,C.C.5.1894,Villa Elisa,Argentina
2Facultad
de Ciencias Astron′o micas y Geof′?sicas,Universidad Nacional de La Plata,La Plata,Argentina
3Australia Telescope National Facility,CSIRO;P.O.Box 76,Epping NSW 1710,Australia
Accepted 2005June 23,Received 2005June 22;in original form 2005March 23
ABSTRACT
We analyze the distribution of the interstellar matter in the environs of the Wolf-Rayet star LSS 3982(=WR 85,WN6+OB?)linked to the optical ring nebula RCW 118.Our study is based on neutral hydrogen 21cm-line data belonging to the Southern Galactic Plane Survey (SGPS).
The analysis of the H i data allowed the identi?cation of a neutral hydrogen in-terstellar bubble related to WR 85and the 25′-diameter ring nebula RCW 118.The H i bubble was detected at a systemic velocity of –21.5km s ?1,corresponding to a kinematical distance of 2.8±1.1kpc,compatible with the stellar distance.The neutral
stucture is about 25′
in radius or 21±8pc,and is expanding at 9±2km s ?1.The asso-ciated ionized and neutral masses amount to 3000M ⊙.The CO emission distribution depicts a region lacking CO coincident in position and velocity with the H i structure.
The 9.′
3-diameter inner optical nebula appears to be related to the approaching part of the neutral atomic shell.The H i void and shell are the neutral gas counterparts of the optical bubble and have very probably originated in the action of the strong stellar wind of the central star during the O-type and WR phases on the surrounding interstellar medium.The H i bubble appears to be in the momentun conserving stage.Key words:ISM:bubbles –stars:Wolf-Rayet –ISM:H ii regions
1INTRODUCTION
Wolf-Rayet (WR)stars are the evolutionary descendents of massive O-type stars.With mass loss rates in the interval (1-5)×10?5M ⊙yr ?1and terminal velocities of 1000-3000km s ?1(van der Hucht 2001;Cappa et al.2004),these hot and luminous stars are one of the most powerful stellar wind sources in our Galaxy.Of-type stars are also characterized by high mass loss rates and terminal velocities (Lamers &Leitherer 1993;Prinja,Barlow &Howarth 1990).
The mechanical energy released to the interstellar
medium (ISM)during the WR phase only (t W R
yr,Meynet &Maeder 2003)is in the range (1-30)×1050erg,comparable to the mechanical energy injected during a su-pernova explosion.Both the mass ?ow from the WR star and the previous O-type star phases strongly modify the energetics,the morphology and the chemical abundances of the ISM in the environs of the star.
The interaction of the strong stellar winds with the
?
Fellow of CONICET,Argentina E-mail:pete@https://www.wendangku.net/doc/fb18218716.html,.ar
?Member of Carrera del Investigador,CONICET,Argentina
surrounding interestellar matter has been analyzed by sev-eral authors,taking into account di?erent enviroments (e.g.Garc ′?a-Segura &Mac Low 1995).The stellar ?ow sweeps up the surrounding material creating interstellar bubbles ,which are detected at di?erent wavelengths from the UV to the ra-dio range.In the optical regime,these structures are gener-ally observed as ?lamentary ring nebulae in the light of H αand [O iii ](e.g.Chu et al.1983;Marston et al.1994).They are related to many WR stars and to a relatively large num-ber of O and Of stars.Shell-shaped structures created by stellar winds from massive stars are also identi?ed in the far infrared and in the thermal radio continuum emission (e.g.Mathis et al.1992;Cappa,Goss &Pineault 2002).
Interstellar bubbles appear as cavities and expanding shells in the neutral hydrogen 21cm line emission distri-bution (e.g.Cappa et al.2003and references therein).H i bubbles are external to their optical and radio continuum counterparts,and expand at relatively low velocities (
km s ?1
).In most of the cases the derived dynamical ages are larger than the duration of the WR phase,suggesting that the stellar winds of the massive O-type star progenitor has also contributed to creating the structures.
As part of a systematic search for neutral gas bubbles
2J.Vasquez,C.Cappa and N.
McClure-Gri?ths
Figure 1.H αimage in (α,δ)coordinates showing the two con-centic rings around WR 85(taken from Marston et al.1994).North is up and East is to the left.
around massive stars,we present here a study of the ISM sur-rounding WR 85(=HD 155603B =LSS 3982)based mainly on H i 21cm-line data belonging to the Southern Galactic Plane Survey (SGPS)and additional molecular and radio continuum data.
WR 85is classi?ed as WN6h +OB?.Di?erent distance estimates have been published for this star.WR 85belongs to the HD 155603group,for which Mo?at &FitzGerald (1977)?nd a distance of 1.8kpc.Conti &Vacca (1990)and van der Hucht (2001)locate the star at d =3.7±1.3and 4.7±2.3kpc,respectively,while Hipparcos measure-ments indicate 1.7kpc.The X-ray point like source 1WGA J1714.4-3949coincides in position with the WR star (Pfe?ermann &Aschenbach 1996).
HD 155603B is associated with the optical ring nebula
RCW 118,of about 25′
in diameter (Chu &Tre?ers 1981;Heckathorn,Bruhweiler &Gull 1982,Marston et al.1994;Marston et al.1994b).Chu et al.1983observed RCW 118with the Curtis-Schmidt-0.6m telescope at CTIO in H α,[O iii ]λ5007and [S ii ]λ6730.These authors found that the ionized gas in the nebula has a LSR velocity of –15km s ?1,
and derived an expansion velocity <=
10km s ?1and a dy-namical age of 6.7×105yr,compatible with the duration of the WR phase.Based on the velocity of the ionized gas and on standard galactic rotation models,they estimated a kinematical distance d k ～2.3kpc.
Marston et al.(1994)reobserved the nebula using the same telescope.Their H αimage reveals the presence of two
semi-circular rings.The inner ring has a diameter of 9.′
3and is centered on the WR star,whereas the outer one,25′in diameter,is centered slightly to the south and south-east of the star.The two concentric structures can be clearly identi?ed in the H αimage displayed in Figure 1.
RCW 118is in the same line of sight to the SNR G347.3–0.5,discovered in the rosat All Sky Survey (RASS)by Pfe?ermann &Aschenbach (1996).This SNR,1?in diame-ter,is located at ≈6kpc (see Lazendic et al.2004).
Table 1.H i data:main observational parameters
2DATABASES
The H i 21cm-line emission data used in this paper be-long to the Southern Galactic Plane Survey (SGPS)(McClure-Gri?ths et al.2005)obtained with the Autralia Telescope Compact Array (ATCA)and the Parkes radiote-lescope (short spacing information).The H i data cube is centered at (l,b,v )=(347?14′,–0?29′,–40km s ?1),covers a region of about 2?×2?around the WR star,and has a
synthesized beam of 2.′6×2.′
1.To improve the S/N ratio we applied a Hanning smoothing to the individual line images.Consequently,the original rms noise level of
2.4K was low-ered to 1.3K and the channel velocity resolution was dou-bled.The main observational parameters of the ?nal data cube are summarized in Table 1.
Additional infrared,radio continuum and molecular data were also analyzed.High resolution infrared images (HIRES)were obtained from IPAC 1.The iras data,ob-tained at 12,25,60and 100μm,have angular resolutions
in the range 0.′
5to about 2′.Radio continuum data at 2.4GHz were obtained from the survey by Duncan et al.(1995)
with an angular resolution of 10.′
4.The molecular data cor-responds to the CO (J =1→0)line at 115GHz and belong to the CO survey by Dame et al.(2001),with angular and velocity resolutions of 9′and 1.3km s ?1,respectively,and a rms noise of 0.3K.
3IONIZED AND NEUTRAL GAS DISTRIBUTION TOW ARDS WR 853.1
H i line emission distribution
The strong stellar winds from massive stars are expected to sweep-up the interstellar material around the wind source and to create a highly evacuated region surrounded by an expanding shell.If the ionizing front is trapped within the envelope,the void and the surrounding shell are expected to appear as a region lacking neutral material encircled by regions of enhanced H i emission.The analysis of the neu-tral gas emission distribution in the environs of these stars allows identi?cation of such cavities and surrounding shells associated with the wind sources.
The criteria adopted to relate an H i cavity and shell to a certain star are:(i)the star should be located close to the centre of the void or within the inner border of the H i surrounding shell;(ii)the ionized ring nebula,if present,should appear projected within the cavity or close to the inner border of the neutral shell;and (iii)the kinematical
1
IPAC is fouded by NASA as part of the IRAS extended mission under contract to Jet Propulsion Laboratory (JPL)and California Intitute of Technology (Caltech).
H i bubble around WR 85and RCW 118
3
distance to the H i structure should be compatible,within errors,with the stellar distance.
To facilitate the visualization of the general character-istics of the H i emission in the line of sight to this region of the Galaxy,we show the average H i pro?le corresponding to an area of 1?×1?centered at the position of WR 85in the top panel of Figure 2.The bottom panel shows a plot of the kinematical distance d k versus the LSR radial velocity for the galactic longitude l =
347?,as obtained from the circular galactic rotation model by Brand &Blitz (1993)
Brightness temperatures higher than a few K are ob-served for velocities spanning the range –130to +50km s ?1.According to the quoted circular galactic rotation model,gas at negative velocities is placed at kinematical distances d k ≈0?7kpc or d k >=9kpc,while positive velocities are for-bidden for distances closer than 17kpc.Gas within the near distance range is most probably related to the Local and the Carina-Sagittarius arms (Georgelin &Georgelin 1976).
To analyze in some detail the neutral atomic gas distri-bution in the environs of the WR star,we obtained a series of H i line images at constant velocities,paying particular attention to the gas distribution at negative velocities.The analysis of the neutral atomic gas distribution within the velocity range –150to 0km s ?1shows a clear void with the star projected close to its centre at velocities of about –21km s ?1.
The top panel of Figure 3displays the H i column den-sity distribution within the velociy interval –28.0to –16.5km s ?1,where the void clearly detected.The void appears surrounded by an almost circular shell.The centroid of the structure,de?ned following the maxima in the shell,is
placed at (l,b )=(347?26′,–0?37′
),close to the position of WR 85(indicated by the star symbol).The brightness tem-perature gradient of the structure is slightly steeper towards the galactic plane than towards the other sections of the shell,indicating the presence of higher density regions close to b =0?.
The bottom panel of Fig.3displays a superposition of the H αimage of the region obtained from the Southern H-alpha Sky Survey Atlas (SHASSA)(Gaustad et al.2001)(greyscale )and the same H i contours of the top panel.The 25′
-diameter outer nebula is clearly detected in the optical
image (see Fig.1for a comparison),while the 9.′
3-diameter inner nebula is barely identi?ed.The bottom panel of Fig.3shows that the 25′-diameter optical nebula is projected onto the H i cavity and close to the inner border of the H i shell.
The systemic velocity of the structure,de?ned as the velocity at which the H i cavity presents its largest dimen-sions and deepest temperature gradient,is v sys ≈?21km s ?1.This value is compatible,within errors,with the veloc-ity of the ionized gas found by Chu &Tre?ers (1981)(–15km s ?1).
The presence of the outer optical nebula close to the in-ner border of the H i shell and the morphological agreement between the RCW 118and the H i emission,along with the agreement between the systemic velocity of the H i struc-ture and the velocity of the ionized gas indicate that the H i feature is related to RCW 118.
Figure 4displays two pro?les showing the H i column
density versus the galactic longitude for b =–0?36′
(thin
line )and the galactic latitude for l =347?25′
(thick line ).
d (K p c )
LSR velocity (km/s)
?200
?150
?100
?50
50
100
Figure 2.Top panel:Average H i brightness temperature spec-trum versus LSR velocity,corresponding to an area of 1?×1?centered at the position of WR 85.Bottom panel:Kinematical distance versus LSR velocity plot obtained from the analytical ?t to the circular galactic rotation model by Brand &Blitz (1993)for l =347?.
This plot clearly shows that the WR star is projected onto a minimun in the H i emission distribution.The neutral shell is identi?ed with arrows.The wide line shows that although most of the neutral gas near b =0?is linked to the Sagittar-ius arm,it is unconnected to the H i feature shown in Fig 3.
We analyzed is some detail the H i gas distribution in the
close environs of the 9.′
3optical ring.The top panel of Fig.5displays the neutral gas emission distribution for the velocity interval –29.3to –27.6km s ?1(in grey scale and coutour lines),while the bottom panel shows an overlay of the optical image (grey scale)and the H i emission distribution (contour lines).The ?gure reveals the presence of neutral gas emission closely bordering the inner semi-circular optical ring.The morphological correlation between the H i emission and the border of the inner nebula suggests that the ionized and the neutral material are related.Some correlation between the inner optical ring and neutral hydrogen is also detected at velocities spanning the range –27.6to –25.2km s ?1.This
4J.Vasquez,C.Cappa and N.
McClure-Gri?ths
Figure 3.Top panel:H i column density distribution surrounding WR 85within the velocity interval –28.0to –16.5km s ?1.The grayscale corresponds to (1.2-1.7)×1021cm ?2and the contour lines are 1.2,1.4,1.5and 1.6×1021cm ?2.The star symbol indi-cates the position of the WR star.Bottom panel:Overlay of the shassa H αimage of the nebula and the same H i contours of the top panel.H αunits are arbitrary.
H i gas is also shown as the H i peaks interior to the H i
shell detected about 10′far from the star in the pro?les in Fig.4.
The velocity interval at which the correlation between the inner ring and the H i cloud is better detected suggests that the inner optical nebula is located on the approaching section of the expanding shell associated with RCW 118.3.2
Radio continuum emission
Figure 6displays an overlay between the radio continuum emission at 2.4GHz (contour lines)and the H i column den-sity distribution (greyscale).Within the region of interest,
the ?gure shows a radio source centered at (l,b )=(347?32′
,
–0?29′
),coincident with the brightest section of RCW 118and with the inner optical ring located close to the star.Weak radio emission can also be detected toward higher negative galactic latitudes and lower galactic longitudes,co-
Figure 4.Pro?les showing the H i column density within the velocity interval –28.0to –16.5km s ?1versus galactic longitude
obtained at b =–0?36′
(thin line)and versus galactic latitude at l =347?25′(thick line).The x-axis is referred to the stellar position.
incident with fainter regions of RCW 118.The positional coincidence between both the radio source and the weak ra-dio emission,and RCW 118suggests that the emission at 2.4GHz originates in the ionized nebular gas.
An image at 4.85GHz can be obtained from the PMN Survey (Condon,Broderick &Seielstadet 1995).However,the presence of extended areas lacking radio data within the region of interest does not make this image useful.The presence of weak radio emission in this region is also evident at 4.85GHz in the survey by Haynes,Caswell &Simonset (1978).
3.3Molecular and IR emission
The left panel of Figure 7shows the CO(J=1→0)line emis-sion distribution within the velocity range –32.5to –24.7km s ?1taken from the Dame et al.(2001)survey.The stellar position is indicated by the star.A region of low molecu-lar emission,～1?30′×0?45′in size,centered near (347?25′,–0?36′)is evident in the image.The right panel of the ?g-ure displays an enlargement of the molecular void showing an overlay of the CO emission distribution (thick contour lines)and the H i column density image of Fig.3(grayscale and thin contour lines).
The image on the right shows the clear correspondence between the H i structure and the higher galactic longitude
section of the CO cavity (l >347?00′
).Note that the CO maxima are external to the H i shell,suggesting that some strati?cation in the gas density is present.The section of the
molecular cavity at l <347?00′
,which is wider in galactic latitude,is not linked to the interstellar bubble.
The hires iras images at 12,25,60and 100μm do not show any structure connected either to the optical or to the H i and CO shells.Only an IR emission gradient probably
H i bubble around WR 85and RCW 1185
G A L A C T I C L A T .
GALACTIC LONG.
347 40
3020-00 2535
45G A L A C T I C L A T .
GALACTIC LONG.
347 40
3020-00 25
35
45Figure 5.Top panel:H i emission distribution within the velocity interval –29.3to –27.6km s ?1in grey scale and contour lines.The grey scale corresponds to 45to 90K.The contour lines are 45,50,53,55K.The cross marks the position of the WR star.Bottom panel:Overlay of the shassa H αimage and the same H i contours of the top panel.
linked to the galactic plane is present in the images at 60and 100μm.
Figure 6.Overlay of the radio continuum image at 2.4GHz (con-tour lines)and the H i column density distribution (grayscale).The star marks the position of WR 85.Contour lines are 0.04,0.09,0.1,0.27,0.29and 0.32Jy.
4THE H i BUBBLE RELATED TO WR 85AND RCW 1184.1
The distance
The kinematical distance d k to the H i structure was esti-mated from the analytical ?t to the circular galactic rotation model Brand &Blitz (1993).
This model predicts that gas at v sys =–21km s ?1should be located at 2.7±0.7kpc or 14±1kpc.The uncer-tainties in the quoted values were estimated by assuming the presence of non-circular motions of ≈6km s ?1.The near kinematical distance estimate is compatible with the kine-matical distance of the ionized gas (d k =2.0kpc)derived using the same model.
Bearing in mind the available photometric data for WR 85and the intrinsic color and absolute magnitude cor-responding to a WN 6star from van der Hucht (2001),the spectrophotometric distance estimate is d ≈2.2±0.9kpc,where the uncertainty in the stellar distance corresponds to the error in the absolute magnitude (±0.9mag).This dis-tance estimate is consistent with the near kinematical dis-tance derived from H i data.
van der Hucht (2001)suggests the existence of an OB companion to WR 85.However,the absence of OB absorp-tion lines in the spectrum of WR 85(Gamen,private com-munication)suggests that the OB companion would be at least 2.5mag weaker than the WR star.Consequently,a correction factor to the apparent magnitude of WR 85has not been taken into account.
Bearing in mind these values and the distances derived by di?erent authors (see §1),we adopted d k =2.8±1.1kpc for both the optical and the H i structures.The uncertainty in the adopted distance is 40%.
The agreement in position,velocity and distance among the WR star,RCW 118and the H i feature suggests that the H i structure is associated with the outer optical ring nebula.
6J.Vasquez,C.Cappa and N.McClure-Gri?ths
Table2.Physical parameters of the HI bubble
The presence of a central star characterized by a strong mass ?ow inside the H i structure and the optical nebula suggests that the stellar wind of the WR star and its massive progen-itor may have had an important role in shaping the nebula. We therefore interpret the H i structure as the neutral gas counterpart of the optical interstellar bubble.
4.2Main parameters of the interstellar bubble
around WR85
The physical parameters of the H i bubble are summarized in Table2.The centroid of the structure was de?ned taking into account the position of the maxima in the shell.
The velocity range corresponds to the velocity inter-val where the structure is detected.The systemic velocity was de?ned in§3.1The expansion velocity was estimated as v exp=(v2?v1)/2+1.6km s?1and represents a lower limit to the true expansion velocity.The extra1.6km s?1allows for the presence of H i in the undetected caps of the expand-ing shell.Because of its small column density,these caps are di?cult to identify in the fore-and background emission.
The cavity was de?ned following the contour line corre-sponding to1.4×1021cm?2(see Fig.3).The angular radius of the shell corresponds approximately to the outer border of the envelope.It can be clearly established for b<–0?25′, while confussion with fore-and background gas precludes the identi?cation of the shell near b<–0?10′.The size of the bubble was estimated through the maxima in the shell.
The H i mass de?ciency in the cavity and the H i mass in the shell were obtained from the column density image shown in Fig.3.The swept-up neutral mass associated with the H i bubble was derived as a mean value between the mass de?ciency in the cavity and the mass in the shell assuming a10%He abundance.
Bearing in mind an error of40%in the adopted dis-tance,uncertainties in radii and masses are about40%and 80%,respectively.
Evolutionary models of interstellar bubbles allow an es-timate of the dynamical age as t d=0.50×106R/v exp yr (McCray1983),corresponding to the momentum conserv-ing stage of an interestellar bubble,where R is the radius of the bubble(pc),v exp is the expansion velocity(km s?1) and the constant is the deceleration parameter,which cor-responds to a mean value between the energy and the mo-mentum conserving cases.The derived dynamical age t d=1.1×106yr,is larger than the duration of the WN phase of
a massive star(t W N=0.3×106yr for a rotating star of40 M⊙,Meynet&Maeder2003)and suggests that the O-type star progenitor of the present WR star has contributed in the formation of the bubble.
A rough estimate of the ionized mass M i and the elec-tron density n e related to RCW118were obtained from the radio continuum image at2.4GHz(Fig.6)using the classi-cal expressions by Mezger&Henderson(1967)for the case of a spherical H ii region.We derived the?ux density by assuming that the strong radio source at347?32′,–0?29′and part of the weak radio emission towards higher negative galactic latitudes and lower galactic longitudes are related to RCW118.For a?ux density S2.4=12Jy,and assuming an electron temperature of104K,and a?lling factor f= 0.35-0.45,we derived M i=2100–2400M⊙and n e=13–15cm?3.The?lling factor was estimated from the optical image and corresponds to an ionized shell of about13′in radius and4′in thickness.We assume that about50-70% of the shell surface is covered by gas.Uncertainties in the ionized masses and electron densities are about80%.We have also assumed that He is singly ionized.
Taking into account the neutral atomic and the ion-ized masses,the total mass in the interstellar bubble is M s～3000M⊙.The average ambient density estimated by distributing the total mass within a volume of21pc in radius is～3cm?3.
It is not clear whether part of the molecular mate-rial that encircles both the H i and H ii shells participates in the expansion.An estimate of the amount of molecular gas can be obtained from Fig.7by applying the empiri-cal relation between W CO(= T mb dv)and the H2column density N H
2
=(1.1±0.2)×1020×W CO cm?2(K km s?1)?1, obtained fromγ-ray studies of molecular clouds in the IV galactic quadrant(Slane et al.1999).The total H2mass is estimated to be6800M⊙.
4.3The energetics
An estimate of the mechanical luminosity L w(=˙M V2w/2) of the stellar wind of WR85can be obtained by assuming a typical mass loss rate˙M=2×10?5M⊙yr?1for the WN phase(Cappa et al.2004)and a terminal velocity V w=1430 km s?1(Rochowicz&Nieldzieski1995).For the previous main sequence O-type star phase,we adopted˙M=2×10?6 M⊙yr?1and a terminal velocity V w=1000km s?1(Prinja, Fullerton&Crowther1996).Mechanical luminosities corre-sponding to the WR and the O-type star phases turn out to be L W R=1.3×1037erg s?1and L O=6.3×1035erg s?1.As-suming a typical lifetime for the WN phase t W N=0.3×106 yr(Meynet&Maeder2003)and for the O-type phase t O =3×106yr(Conti&Vacca1990),the total stellar wind mechanical energy transferred to the ISM is E w=1.8×1050 erg.A similar value(1.2×1050erg)is derived asuming that the stellar wind of the WR star and the previous O-type star phase have blown the gas bubble during0.3×106and 0.8×106yr,respectively.These lifetimes are compatible with the derived dynamical age.Taking into account the large un-certainty in the dynamical age,we believe that the derived E w-values can be considered as the lower and upper limits to the true stellar wind energy.
The kinetic energy E k(=M s V2exp/2)in the interstellar
H i bubble around WR85and RCW118
7
Figure7.Left panel:.Mean brightness temperature corresponding to the CO emission distribution within the velocity interval–32.5to –24.7km s?1.The grey scale corresponds to0.2to1.7K.The contour lines are0.3,0.5and0.9K.The cross marks the position of the WR star.The triangles mark the location of iras protostellar candidates(see text).Right panel:Enlargement of the central region of the image on the left showing an overlay of the H i(grayscale and thin contour lines)and the CO(thick contour lines)emissions.The star symbol indicates the stellar position.The triangles mark the location of iras protostellar candidates.
bubble derived taking into account the expansion velocity from Table2and the swept-up atomic neutral and ionized masses,is E k=8.3×1048erg.If the molecular material also participates in the expansion,E k=8.8×1048erg.
The ratio?(=E k/E W)is in the range0.005-0.03. These values indicate that the central star is capable of blow-ing the interstellar bubble.The?gure derived for WR85is similar to the ones obtained for most of the H i interstellar bubbles found around O-and WR-stars.These values sup-port the interpretation that bearing in mind the standard energy conserving model by Weaver et al.(1977),the ob-served stellar wind energy appears to be too high for the observed bubble dynamics,as pointed out by Cooper et al. (2004),and suggest that the bubbles are most probably in the momentum conserving stage.However,the drain of en-ergy from the bubble through the patchy envelope can not be ruled out.
The ambient density obtained by distributing the total mass within the volume of the bubble(see§4.2)is compat-ible with the value derived for the momentum conserving case(～3cm?3).
The SNR G347.3-0.5is seen projected onto the same area.The derived distance to the SNR,d=6kpc,based on molecular line information(Slane et al.1999),precludes any relation between the SNR and RCW118and the H i shell. 5CONDITIONS FOR STAR FORMATION
The high velocity mass?ow produces a drastic change in the physical conditions of the surrounding ISM.Shock fronts linked to stellar winds from massive stars may induce star formation in the high density regions of the neutral shells, where material has accumulated and conditions for star for-mation may have been favoured.Then,it is important to analyze the presence of star formation indicators in the neu-tral shells.
Since protostellar candidates can be identi?ed as in-frared sources in the iras Point Source Catalogue,we per-formed a search for iras point sources projected onto a re-gion of3?in size centered at the stellar position whose en-ergy distributions are compatible with protostellar objects according to the criteria listed by Junkes,F¨u rst&Reich (1992).The IR sources found in our search are indicated by triangles in Fig.7(left panel).Only the ones within an area of1?in radius centered at the WR position(triangles with numbers)are listed in Table3,which shows the source number,its iras number identi?cation,and the?uxes in the four iras bands.
It is clear from the left panel of the?gure that most of the sources are projected onto regions of strong CO emission or close to the galactic plane.The triangles in the right panel of Fig.7mark the position of iras point sources.This panel shows the close correspondence between the IR sources2,3, 6,14,15,17and18,and the molecular and H i shells linked to RCW118,suggesting that sequential star formation may be occuring in some sections of the neutral envelope,where conditions for stellar formation might have been developed. We note that the distances to these sources are unknown. 6SUMMARY
We have analyzed21cm line data belonging to the Southern Galactic Plane Survey searching for an H i bubble related to WR85and its ring nebula RCW118.The main results of our search can be summarized as follows:
(i)The H i data allowed the identi?cation of a cavity in the neutral gas distribution surrounded by a slowly expanding shell.The structure was detected at velocities spanning the
8J.Vasquez,C.Cappa and N.McClure-Gri?ths
Table3.Protostellar candidates within a region of1?in radius
centered on WR85
#l b iras F(12μm)F(25μm)F(60μm)F(100μm)
designation
(?′)(?′)(Jy)(Jy)(Jy)(Jy)(Jy)
interval–28.0to–16.5km s?1,and has a systemic velocity of–21±5km s?1.The cavity can also be identi?ed in the CO emission distribution at similar velocities.
(ii)The ring nebula RCW118appears projected onto the inner border of the H i shell.
(iii)The systemic velocity of the H i structure is similar to the velocity of the ionized gas in RCW118.
(iv)WR85is seen in projection onto the central part of the H i cavity and close to its geometrical center.
(v)The coincidence,within errors,of the kinematical dis-tance to the H i structure and the stellar distance strongly suggests that the WR star is placed within the cavity. (vi)The morphological coincidence between the inner op-tical nebula and the H i emission at about–28km s?1sug-gests that the9.′3nebula is located on the approaching part of the expanding shell.The WR star,which appears closely related to the inner nebula,is also probably located near the approaching part of the shell.
(vii)The CO emission distribution reveals the presence of a molecular shell almost encircling the HI envelope. (viii)The position of the iras protostellar candidates pro-jected onto the molecular shell,suggests that star formation might be occuring in the region.However,additional studies should be performed to investigate this point.
(ix)The stellar wind of WR85is capable of blowing the observed ionized and neutral structure.
The bulk of evidence(i)to(ix)strongly indicates that the H i structure is the neutral gas counterpart of the optical bubble and shows the action of the stellar winds on the surrounding material.
Adopting a distance of2.8±1.1kpc,the neutral inter-stelar bubble has a linear radius of～21pc.Taking into account an expansion velocity of9±2km s?1,its dynamical age is1.1×106yr,suggesting that both the present WR star and its massive stellar progenitor have contributed in shap-ing the bubble.The associated neutral and ionized masses are3000M⊙,which indicates that the bubble evolved in a medium with an average ambient density of3cm?3. ACKNOWLEDGMENTS
We acknowedge the referee Dr A.P.Marston for many sug-gestions that improved the?nal presentation of this pa-per.We thank Dr.T.Dame for making available to us the CO data,and Dr.R.Gamen for allowing us to use infor-mation on WR85in advance of publication.This project was partially?nanced by the Consejo Nacional de Inves-tigaciones Cient′??cas y T′e cnicas(CONICET)of Argentina under project PIP607/98and FCAG,UNLP under projects 11/G049and11/G072,and Agencia Nacional de Promoci′o n Cienf′??ca y Tecnol′o gica(ANPCYT)under project PICT 14018/03.The Digitized Sky Survey(DSS)was produced at the Space Telescope Science Institute under US Govern-ment grant NAGW-2166.
REFERENCES
Brand J.,Blitz L.1993,A&A,275,67
Cappa C.,Goss W.M.,van der Hucht K.A.,2004,AJ, 127,2885
Cappa C.,Arnal M.,Cichowolski S.,Goss W.M.,Pineault S.2003,IAU Symp.212,A Massive star Odyssey,from Main Sequence to Supernova,p.596
Cappa C.,Goss W.M.,Pineault S.,2002,AJ,123,3348 Chu Y.-H.,Tre?ers R.R.,Kwitter K.1983,ApJS,53,937 Chu,Y.-H.,Tre?ers,R.R.1981,ApJ,250,615
Condon J.J.,Broderick J.J.,Seielstad G.A.,1995,ADIL, JC,6
Conti P.S.,Vacca W.D.1990,AJ,100,431
H i bubble around WR85and RCW1189 Cooper R.L.,Guerrero M.A.,Chu Y.-H.,Rosie Chen C.
-H.,Dunne B.C.,2004,ApJ,605,751
Dame T.M.,Hartmann D.,Thaddeus P.2001,ApJ,547,
792
Duncan,A.R.,Stewart R.T.,Haynes R.F.,Jones K.L.
1995,MNRAS,277,36
Gaustad J.E.,McCullough P.R.,Rosing W.,Van Buren
D.2001,PASP,113,1326
Garc′?a-Segura,G.,Mac Low,M.-M.1995,ApJ,455,145
Georgelin,Y.M.,Georgelin,Y.P.1976,A&A,49,57
Haynes R.F.,Caswell J.L.,Simons L.W.J,1978,AuJPA,
45,1
Heckathorn,J.N.,Bruhweiler F.C.,Gull T.R.1982,ApJ,
252,230
Hunter S.D.,Digel S.W.,de Geus E.J.,Kanback G.,1994,
ApJ,436,216
van der Hucht K.2001,New astronomy Rev.,45,135
Junkes N.,F¨u rst E.,Reich W.,1992,A&AS,261,289
Lamers H.J.G.L.M.,Leitherer C.,1993,ApJ,412,771
Lazendic J.S.,Slane P.O.,Gaensler B.M.,Reynolds S.
P.,Plucinsky P.P.,Hughes,J.P.,2004,ApJ,602,271
Leitherer C,Chapman J.M.,Koribalski B.,1997,ApJ,481,
898
Marston A.P.,Yocum D.R.,Garc′?a-Segura G.,Chu,Y.-H.
1994a,ApJS,93,229
Marston A.P.,Yocum D.R.,Garc′?a-Segura G.,Chu,Y.-H.
1994b,ApJS,95,151
Mathis J.S.,Cassinelli J.P.,van der Hucht K.A.,Prusti
T.,Wesselius P.R.,Williams P.1992,ApJ,384,197
McClure-Gri?ths N.M.,Dickey J.M.,Gaensler B.M.,
Green A.J.,Haverkorn M.,Strasser S.,2005,ApJ,in
press.
McCray R.,1983,HiA,6,565
Meynet G.,Maeder A.2003,A&A,404,975
Mezger P.G.,Henderson A.P.,1967,ApJ,147,471
Mo?at A.F.J.,Fitzgerald M.P.1977,A&A,54,263
Pfe?ermann E.,Aschenbach B.,1996,rftu.proc.,267
Prinja R.K.,Barlow M.J.,Howarth I.D.,1990,ApJ,361,
607
Prinja R.K.,Fullerton A.W.,Crowther P.A.,1996,A&A,
331,264
Rochowicz K.,Nieldzieski A.,1995,AcA,45,307
Slane P.,Gaensler B.M.,Dame T.M.,Hughes J.P.,Plu-
cinsky P.P.,Green A.,1999,ApJ,525,357
Weaver R.,McCray R.,Castor J.,Shapiro,P.,Moore R.,
1977,ApJ,218,377
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配置H3C交换机常用命令
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思科交换机-常用命令及配置 switch> 用户模式 1：进入特权模式enable switch> enable switch# 2：进入全局配置模式configure terminal switch> enable switch＃configure terminal switch(conf)# 3：交换机命名hostname name 以cisco001 为例 switch> enable switch＃c onfigure terminal switch(conf)#hostname cisco001 cisco001(conf)# 4：配置使能口令（未加密）enable password cisco 以cisco 为例switch> enable switch＃configure terminal cisco001(conf)# enable password cisco 5：配置使能密码（加密）enable secret ciscolab 以cicsolab 为例switch> enable switch＃configure terminal switch(conf)# enable secret ciscolab
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在弹出的窗口中点击下图中的按钮 按照下图中选择选项：
选择完成后点击确定按钮后敲击回车，如窗口中显示XXXXX>则说明设备连接成功。 2、配置5750交换机步骤 A、第一步删除5750交换机现有配置，复制下边命令并粘贴到crt命令行内： en ruijie delete config.text y reload y B、重新配置5750交换机： en
conf t hos btjx-zhl-25750-2 vlan 101 exit int vlan 101 ip add 192.168.101.252 255.255.255.0 exit ip route 0.0.0.0 0.0.0.0 192.168.101.254 enable sec ruijie lin vty 0 4 pass ruijie exit rldp enable int r g0/1 – 22 sw mo acc sw acc vlan 101 rldp port loo shutdown-port exit int r g0/23 – 24 me fi sw mo tr int g0/24
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3、常用配置命令 3.1 把端口加入到vlan Switch>en Password: Switch #conf t /*进入配置模式*/ Enter configuration commands, one per line. End with CNTL/Z. Switch (config)#inter f 0/1 /*进入端口*/ Switch (config-if)#switchport access vlan X /*把端口加入到vlan X*/ Switch (config-if)#end Switch #wr /*保存*/ Building configuration... [OK] Switch # 3.2 添加新vlan（在核心交换机上写） Switch>en Password: Switch #conf t /*进入配置模式*/ Enter configuration commands, one per line. End with CNTL/Z. Switch (config)#Vlan X /*添加新Vlan*/ Switch (config-vlan)#inter vlan X /*进入Vlan*/ Switch (config-if)#ip address x.x.x.x 255.255.255.0/*设置vlan ip地址*/ Switch (config-if)#no shut 3.3 配置trunk，透传vlan Switch>en Password: Switch #conf t /*进入配置模式*/ Enter configuration commands, one per line. End with CNTL/Z. Switch (config)#inter fast 0/x /*进入级联端口*/ Switch (config-if)#switchport mode trunk /*修改端口模式*/ Switch (config-if)# switchport trunk allowed vlan all /*设置允许通过的vlan*/ 保存 删除命令：所有的命令前面加no。
小学语文教师个人工作总结
小学语文教师个人工作总结 逝者如斯夫，不舍昼夜。一个学期的工作已经结束，这个学期我担任五年级语文兼班主任工作，一年来，我认真履行教师职责。下面我就从以下几方面谈谈自己的工作。 一、语文教学工作。 在教学中，我刻苦钻研、虚心求教，不断改进自己的教学方式，培养学生良好的学风和学习习惯，帮助学生提高学习质量，培养学生自学和独立思考的能力，在语文教学中渗透思想品德教育。为了让学生掌握最好的学习方法，我在备课中，根据大纲要求，从班级的特点出发，着重突破教学难点，抓住教学重点，创设种种情景，千方百计调动学生的积极性。一切从学生出发，使学生成为学习的主体，务必让每一位学生在一堂课中都能有所收获。因此，在教学中，我总是鼓励学生多讲，多练，大面积铺开，鼓励学习有困难的学生发言，激发他们的学习热情，学习兴趣和求知欲，培养学生的创造力，提高学生的语文素养。 对于学困生的辅导和转化，我赋予教师真诚的爱，暗中给他们鼓励，扬其所长，让他们也体会到学习的兴趣。除此之外，我还组织学生“结对子”，建立学习互助小组，让他们共同进步，既培养了同学之间的团结友爱，也树立了良好的班风、学风。 在不断提倡课程改革的今天，我着力于培养学生的创新能力和实践能力。在这种教学思想的指引下，我也努力探索，大胆尝试，逐渐摸索出了一套适合自己教学的方法，并在教学实践中得到了学生的喜欢以及老师们的肯定。 二、班主任工作方面 在坚持教好书的同时，我从未放弃过育好人。我觉得，做一个班主任也许不难，但要做一个好班主任就很难了。根据我在班主任工作中的经验，我努力做到了两个字：“爱”和“严”，这使我在班主任工作中取得了较好的成绩，既改变了一大批后进生，又培养了一批优秀的学生。 1、有一颗爱心，这是做好工作的前提。 爱学生，就必须善于走进学生的情感世界，就必须把学生当作朋友，去感受他们的喜怒哀乐。爱学生，要以尊重和依赖为前提，要做到严中有爱。我经常从小处着手，从学生关心的事寻求最佳教育时机，给学生春风沐浴般的教育。带着一颗“爱心”去工作，可以让学生觉得你是真心地关心他，缩短了师生之间的距离，同时，他们犯了什么错误，也就容易接受你的教育，很快地加以改正。这种爱，有对学生思想形成的正确引导，更有对学生生活上实实在在的关心。 2、细心、耐心、诚心这是做好工作的基础。
华为的交换机基本配置命令
华为的交换机基本配置命令很多，在此，yjbys小编为大家带来的是最新交换机的配置命令，希望对同学们考试有帮助! 1、配置文件相关命令 [Quidway]display current-configuration 显示当前生效的配置 [Quidway]display saved-configuration 显示flash中配置文件，即下次上电启动时所用的配置文件 reset saved-configuration 檫除旧的配置文件 reboot 交换机重启 display version 显示系统版本信息 2、基本配置 [Quidway]super password 修改特权用户密码 [Quidway]sysname 交换机命名 [Quidway]interface ethernet 1/0/1 进入接口视图 [Quidway]interface vlan 1 进入接口视图 [Quidway-Vlan-interfacex]ip address 10.1.1.11 255.255.0.0 配置VLAN的IP地址 [Quidway]ip route-static 0.0.0.0 0.0.0.0 10.1.1.1 静态路由=网关 3、telnet配置 [Quidway]user-interface vty 0 4 进入虚拟终端 [S3026-ui-vty0-4]authentication-mode password 设置口令模式 [S3026-ui-vty0-4]set authentication-mode password simple xmws123 设置口令 [S3026-ui-vty0-4]user privilege level 3 用户级别 4、端口配置 [Quidway-Ethernet1/0/1]duplex {half|full|auto} 配置端口工作状态 [Quidway-Ethernet1/0/1]speed {10|100|auto} 配置端口工作速率 [Quidway-Ethernet1/0/1]flow-control 配置端口流控 [Quidway-Ethernet1/0/1]mdi {across|auto|normal} 配置端口平接扭接 [Quidway-Ethernet1/0/1]port link-type {trunk|access|hybrid} 设置端口工作模式 [Quidway-Ethernet1/0/1]undo shutdown 激活端口 [Quidway-Ethernet1/0/2]quit 退出系统视图 5、链路聚合配置