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Since the eas temperature is decreasing outward. the larger variation in the location where the radiation originates on the low Irequency. side of the mode leads to a smaller temperature variation there. while the smaller variation in the location where radiation originales on the hieh frequency side of the mode leads to a larger temperature variation there. | Since the gas temperature is decreasing outward, the larger variation in the location where the radiation originates on the low frequency side of the mode leads to a smaller temperature variation there, while the smaller variation in the location where radiation originates on the high frequency side of the mode leads to a larger temperature variation there. |
We therefore observe a Larger intensity variation on the hieh frequency side of the mode than on the low frequency side of the mode ancl (thus the asvinmetry is reversed from (hat observed in the velocity. (and temperature when measured at a fixed geometrical depth). | We therefore observe a larger intensity variation on the high frequency side of the mode than on the low frequency side of the mode and thus the asymmetry is reversed from that observed in the velocity (and temperature when measured at a fixed geometrical depth). |
hat even though the amplitude and in many cases the peak »ositions of the wiggles on the 201 . 201 grid have nearA converged to their values on the 401 401 grid. the shocks on the higher resolution grid have a dillerent. profile. | that even though the amplitude and in many cases the peak positions of the wiggles on the 201 $\times$ 201 grid have nearly converged to their values on the 401 $\times$ 401 grid, the shocks on the higher resolution grid have a different profile. |
μον end to be sharper and to have higher density ancl velocity contrast so that a measurement of the spatial overlap of he wigeles with observations finds significant discrepancies oetween the two models. | They tend to be sharper and to have higher density and velocity contrast so that a measurement of the spatial overlap of the wiggles with observations finds significant discrepancies between the two models. |
Furthermore in comparison with he (lower resolution) observed. gas kinematies the wigeles on the 401 401 erid exhibit larger average deviations [roni he data points. resulting in a worse overall y7/N value. | Furthermore in comparison with the (lower resolution) observed gas kinematics the wiggles on the 401 $\times$ 401 grid exhibit larger average deviations from the data points, resulting in a worse overall $\chi^2/$ N value. |
Accordingly. we argue that simulations should be performed on à grid with a cell size comparable to the spatial resolution of the observational data that they will be compared. to. | Accordingly, we argue that simulations should be performed on a grid with a cell size comparable to the spatial resolution of the observational data that they will be compared to. |
Alternatively one can smooth high-resolution simulations to match the spatial resolution of the observations. | Alternatively one can smooth high-resolution simulations to match the spatial resolution of the observations. |
Finally. to explore the \7/N values resulting from a dillercut and more diffusive hvdrocode. we plotted results from the beam scheme (filled. circles) for simulations with fiducial values for the eric resolution. gas sound speed. ancl pattern speed. | Finally, to explore the $\chi^2/$ N values resulting from a different and more diffusive hydrocode, we plotted results from the beam scheme (filled circles) for simulations with fiducial values for the grid resolution, gas sound speed, and pattern speed. |
Figure 20. shows that the beam scheme seems to work relatively well for most of the disk regions. | Figure \ref{chi} shows that the beam scheme seems to work relatively well for most of the disk regions. |
It should. be noted however that the central region of the disk. where the beam scheme is the least successful. was excluded from the comparison. | It should be noted however that the central region of the disk, where the beam scheme is the least successful, was excluded from the comparison. |
Naivelv reading figure 20.. we would conclude that the 45 per cent. disk. model is the best match to. the observations. | Naively reading figure \ref{chi}, we would conclude that the 45 per cent disk model is the best match to the observations. |
However. in light of section 3. which illustrated the unlikelihood. of simple simulations exactly matching every wigele in the observations. we make the following remarks on the X7E analvsis. | However, in light of section \ref{Parameters} which illustrated the unlikelihood of simple simulations exactly matching every wiggle in the observations, we make the following remarks on the $\chi^2$ analysis. |
Lf for à simulation performed with a given. fy there is a large zunplitude wigele which is slightly spatially shifted from the wigele in the observation. it will give a large deviation in the x7.2 plot. | If for a simulation performed with a given $f_{\rm d}$ there is a large amplitude wiggle which is slightly spatially shifted from the wiggle in the observation, it will give a large deviation in the $\chi^2$ plot. |
As a result. the simulation may be discarded. as one which gives a poor match to the observation when in fact it could. be that the simulation parameters. were reasonable but not precise enough. | As a result, the simulation may be discarded as one which gives a poor match to the observation when in fact it could be that the simulation parameters were reasonable but not precise enough. |
For example. the physical sound: speed. at a wigele location could have been very. dillerent. [rom the simulation sound speed. or the pattern speed which has the ereatest. influence on the positions of the wigeles. is not as constant as modeled. | For example, the physical sound speed at a wiggle location could have been very different from the simulation sound speed, or the pattern speed which has the greatest influence on the positions of the wiggles, is not as constant as modeled. |
On the contrary. the simulations with smaller wigeles. caused either by low disk. fraction. high sound speed. low resolution. or a very dilfusive scheme. | On the contrary, the simulations with smaller wiggles, caused either by low disk fraction, high sound speed, low resolution, or a very diffusive scheme, |
The cuviromment has a strong influence on spiral galaxies evolving iu a cluster. | The environment has a strong influence on spiral galaxies evolving in a cluster. |
The ideal place to study the evolution of cluster spiral galaxies is the Virgo cluster. because it represents the onlv cluster in the northeru hemisphere where one can observe the ISM distribution and kinematics of cluster galaxies at a kpc resolution (Lipe ~1211, | The ideal place to study the evolution of cluster spiral galaxies is the Virgo cluster, because it represents the only cluster in the northern hemisphere where one can observe the ISM distribution and kinematics of cluster galaxies at a kpc resolution (1 kpc $\sim 12''$. |
The Virgo cluster is dynamically young aud spiralrich. | The Virgo cluster is dynamically young and spiral-rich. |
The cluster spiral galaxies have lost up to 90 deficient (Chamaraius et al. | The cluster spiral galaxies have lost up to $90$ deficient (Chamaraux et al. |
1980. Ciovauclli Tavues 1983). | 1980, Giovanelli Haynes 1983). |
Tagine observations have showu that these ealaxies have truncated disks (Caovanclli Tavues 1983. Cavatte et al. | Imaging observations have shown that these galaxies have truncated disks (Giovanelli Haynes 1983, Cayatte et al. |
L990). | 1990). |
Thus. the cluster euvironmoeut changes the coutent and morphology of Virgo cluster spiral galaxies. | Thus, the cluster environment changes the content and morphology of Virgo cluster spiral galaxies. |
However. Virgo spiral galaxies are not or only mikllv CO-deficient (INXeuuev Young 10989: sec. however. Fuimagallii « al. | However, Virgo spiral galaxies are not or only mildly CO-deficient (Kenney Young 1989; see, however, Fumagalli et al. |
2009). | 2009). |
Iu a recent maging survey of Virgo galaxies (VIVA: VLA Tagine of Virgo ealaxies in Atomic HHOris. ‘lane et al. | In a recent imaging survey of Virgo galaxies (VIVA: VLA Imaging of Virgo galaxies in Atomic gas, Chung et al. |
2009). Chung et al. ( | 2009), Chung et al. ( |
2007) found seven spiral galaxies with long ouc-sided ails. | 2007) found seven spiral galaxies with long one-sided tails. |
These ealaxics are ound in mtermediate- to low-density regions (0.6-1 Apc in projection from ΔΙΟΤΙ | These galaxies are found in intermediate- to low-density regions (0.6-1 Mpc in projection from M87). |
, The ails are all )omutiug rougilv awav frou M87. sugeestiug hat these tails are due to run pressure strippiug. | The tails are all pointing roughly away from M87, suggesting that these tails are due to ram pressure stripping. |
Therefore. rau. pressure stripping already. begins to affect Spiral galaxies around fιο cluster) Virial radius. | Therefore, ram pressure stripping already begins to affect spiral galaxies around the cluster Virial radius. |
The urther evolution of a galaxy depeuds critically ou its orbit (sec. e... Voller et al. | The further evolution of a galaxy depends critically on its orbit (see, e.g., Vollmer et al. |
2001). 1.6. a highly cecentric orbit will lead the galaxy at a high velocity iuto the cluster core. where je intrachister οςαι is deusest aud rau pressure will )0 very strong. | 2001), i.e. a highly eccentric orbit will lead the galaxy at a high velocity into the cluster core, where the intracluster medium is densest and ram pressure will be very strong. |
NGC [330 is one of the Virgo spiral galaxies with a oue tail observed by Cline et al. ( | NGC 4330 is one of the Virgo spiral galaxies with a long tail observed by Chung et al. ( |
2007). | 2007). |
It. has a naxinmn rotation velocity of Όρος~180 + and a otal mass of Mig=L5<105 AL. (Chine et al. | It has a maximum rotation velocity of $v_{\rm rot} \sim 180$ $^{-1}$ and a total mass of $M_{\rm HI}=4.5 \times 10^{8}$ $_{\odot}$ (Chung et al. |
2009). | 2009). |
Tt is located at a projected distance of ~2° (600 kpc) from he cluster center. ie. it is relatively close to M 87. and has a radial velocity of 100 ο with respect to the Virgo ucau. | It is located at a projected distance of $\sim 2^{\circ}$ (600 kpc) from the cluster center, i.e. it is relatively close to M 87, and has a radial velocity of 400 $^{-1}$ with respect to the Virgo mean. |
The deficiency of NGC 1330 is 0:8 (Clune et al. | The deficiency of NGC 4330 is $0.8$ (Chung et al. |
2007). | 2007). |
The distribution in the ealactic disk is truncated at about half the optical radius. | The distribution in the galactic disk is truncated at about half the optical radius. |
In addition. NGC 13230 is one of the rare Virgo galaxies showing au extended UV tail (Abramson e al. | In addition, NGC 4330 is one of the rare Virgo galaxies showing an extended UV tail (Abramson et al. |
2011). | 2011). |
The and UV tails show a senificaut offset. with the tail being downwind of the UV tail. | The and UV tails show a significant offset, with the tail being downwind of the UV tail. |
At the cading edge of the interaction. the IIa enission ald dus extinction distribution is bent sharply out ofthe galactic disk. | At the leading edge of the interaction, the $\alpha$ emission and dust extinction distribution is bent sharply out of the galactic disk. |
These features are sigus of active ral pressure stripping. | These features are signs of active ram pressure stripping. |
For a comprehensive description of NGC 1330s optical. UV. and data see Abramson et al. ( | For a comprehensive description of NGC 4330's optical, UV, and data see Abramson et al. ( |
2011). | 2011). |
These authors sugeestOO a secnario in which NCC 1330 is falling iuto the cluster ceuter for the first time and has experienced a significant iucrease in rani pressure Over the last 900-100 My. | These authors suggest a scenario in which NGC 4330 is falling into the cluster center for the first time and has experienced a significant increase in ram pressure over the last 200-400 Myr. |
Iu the ram pressure stripping time sequence of Vireo cluster galaxies. Volhner (2009) has classified NGC 1330 as a case of pre-peak rai pressure stripping together with NGC 501. | In the ram pressure stripping time sequence of Virgo cluster galaxies, Vollmer (2009) has classified NGC 4330 as a case of pre-peak ram pressure stripping together with NGC 4501. |
This evolutionary stage is consistent with a ealaxy orbit leading the galaxy to its closest approach (620 kpc} of the cluster center (M 87) in ~100 Myr. | This evolutionary stage is consistent with a galaxy orbit leading the galaxy to its closest approach (620 kpc) of the cluster center (M 87) in $\sim 100$ Myr. |
Iu this article we preseut new CO aud 6 cum radio continui observations of NGC 13230 and eive the details of the numerical simulations aud eive au explanation for the observed offset between the aud UV tails. which is due to the decoupling of deuse collapsing Reeas clouds from the ran pressure wind. | In this article we present new CO and 6 cm radio continuum observations of NGC 4330 and give the details of the numerical simulations and give an explanation for the observed offset between the and UV tails, which is due to the decoupling of dense collapsing gas clouds from the ram pressure wind. |
The articleis structured in the following wav: the dynamical model is described in Sec. | The articleis structured in the following way: the dynamical model is described in Sec. |
with the best fit model preseuted in Sec. 3.. | \ref{sec:model} with the best fit model presented in Sec. \ref{sec:bestfit}. . |
The | The |
One of the major issues in star formation is understanding the physical conditions. including the temperature and density structure.A of the material out of which stars will form. | One of the major issues in star formation is understanding the physical conditions, including the temperature and density structure, of the material out of which stars will form. |
While fundamental.c these quantities are difficult to determine. | While fundamental, these quantities are difficult to determine. |
These regions are cold and therefore radiate energy away through d=st at the far infrared/submillimeter wavelengths. a frequency range barely accessible from the ground because of the opacity of the atmosphere. | These regions are cold and therefore radiate energy away through dust at the far infrared/submillimeter wavelengths, a frequency range barely accessible from the ground because of the opacity of the atmosphere. |
For the first time. a high angular resolution view of the Liverse from 70 to 500 lis now becoming available thanks to the ESA Herschel Space Observatory (?). | For the first time, a high angular resolution view of the Universe from 70 to 500 is now becoming available thanks to the ESA Herschel Space Observatory . |
. The frequency range provided by its two photometry instruments PACS and SPIRE perfectly matches the emission peaks of young stellar objects and prestellar cores. the direct progenitors of stars. | The frequency range provided by its two photometry instruments PACS and SPIRE perfectly matches the emission peaks of young stellar objects and prestellar cores, the direct progenitors of stars. |
It is now possible to construct well constrained SEDs for these objects. and therefore determine the spatial distributions of the temperature and column density towards a wide range of different objects. | It is now possible to construct well constrained SEDs for these objects, and therefore determine the spatial distributions of the temperature and column density towards a wide range of different objects. |
Hi-GAL ts the open time key project to observe the inner part (f|xοι 1%) of the Galactic. plane with Herschel(2). | Hi-GAL is the open time key project to observe the inner part $|l|\leq60\degr; |b| \leq1\degr$ ) of the Galactic plane with Herschel. |
. The sensitivity of this survey will allow the detection of 10 M. molecular clouds at a distance of 4 kpe. | The sensitivity of this survey will allow the detection of 10 $_{\odot}$ molecular clouds at a distance of 4 kpc. |
A large number of diverse studies will result from this survey covering scientific themes such as evolved stars. diffuse interstellar medium. and star formation. | A large number of diverse studies will result from this survey covering scientific themes such as evolved stars, diffuse interstellar medium, and star formation. |
In this Letter. we present the first Herschel study analyzing the temperature and column density structure of infrared dark clouds (IRDCs). | In this Letter, we present the first Herschel study analyzing the temperature and column density structure of infrared dark clouds (IRDCs). |
These objects are reservoirs of cold. dense molecular gas seen in extinction in the mid-infrared against the strong background emission of the Galactic. planeDmainBodyCitationEnd|peraultI996. | These objects are reservoirs of cold, dense molecular gas seen in extinction in the mid-infrared against the strong background emission of the Galactic plane. |
rathborne2006. This gas is only slightly processed by current star formation activity and most likely still contains the mitial conditions of star formation imprinted within them. | This gas is only slightly processed by current star formation activity and most likely still contains the initial conditions of star formation imprinted within them. |
Their study can therefore illuminate the earliest stages of star formation. | Their study can therefore illuminate the earliest stages of star formation. |
In Sect. | In Sect. |
2 of this paper. we describe the data. Sect. | 2 of this paper, we describe the data, Sect. |
3 focuses on the background properties. | 3 focuses on the background properties. |
Section 4 presents the first results. while Sects. | Section 4 presents the first results, while Sects. |
5 and 6 summarize the discussion and conclusions of the paper. respectively. | 5 and 6 summarize the discussion and conclusions of the paper, respectively. |
This analysis uses data from the Hi-GAL Science Demonstration Phase (SDP) which consists of two tiles of ~2.2?x centered on /=30° and /=59°, | This analysis uses data from the Hi-GAL Science Demonstration Phase (SDP) which consists of two tiles of $\sim 2.2\degr\times2.2\degr$ centered on $l=30\degr$ and $l=59\degr$. |
For each tile. the parallel mode of observations provides PACS 70/160 and SPIRE 250/350/500 images. | For each tile, the parallel mode of observations provides PACS 70/160 and SPIRE 250/350/500 images. |
The SDP data were reduced using the ROMAGAL data reduction software (see | The SDP data were reduced using the ROMAGAL data reduction software (see |
linear. trend of. —1847—pras/claw: the ras. of. the residuals. is. 16.µας. and the reduced 1.1. | linear trend of $-18 \pm 7~\mu$ as/day; the $r.m.s.$ of the residuals is $16~\mu$ as, and the reduced $\chi^2 = 1.1$ . |
The predicted change in differential declination due to orbital motion is approximately —]11 pasdax. | The predicted change in differential declination due to orbital motion is approximately $-11~\mu$ as/day. |
We have achieved an astrometric measurement precision of zz9 µας in 10 minutes of observation on (he 0.25 arcsecond separation binary star ID 171779. | We have achieved an astrometric measurement precision of $\approx 9$ $\mu$ as in 70 minutes of observation on the 0.25 arcsecond separation binary star HD 171779. |
The measurements were repeated on four nights. vielding answers consistent at the level of 16pas. | The measurements were repeated on four nights, yielding answers consistent at the level of $16~\mu$ as. |
These early results show the promise of very narrow-angle astrometry for achieving verv hieh precision nmeasurenientis of stellar binaries wilh a separations on the order of 0.051 areseconds. | These early results show the promise of very narrow-angle astrometry for achieving very high precision measurements of stellar binaries with a separations on the order of 0.05–1 arcseconds. |
This is particularly useful in searching lor planets around such binaries. although (hie resulting visual orbits for these stars should also be useful in providiug stellar masses ancl distances at the level of 10.7. | This is particularly useful in searching for planets around such binaries, although the resulting high-precision visual orbits for these stars should also be useful in providing stellar masses and distances at the level of $10^{-3}$. |
It should be noted that such high precision mass determinations nmav require an extended period of observation as these svstemis can have very long orbital periods. | It should be noted that such high precision mass determinations may require an extended period of observation as these systems can have very long orbital periods. |
It is also necessary to obtain radial velocity data accurate to 10 m/s or better. which can be challenging. | It is also necessary to obtain radial velocity data accurate to 10 m/s or better, which can be challenging. |
This newly demonstrated approach to narrow-angle astromeltry compares quite lavorably with other astrometric methods used to date. such as speckle interferometry (Llorsehetal.Woitasοἱal. 2003).. single-telescope astrometry wilh (Laneetal.2001) and without (Pravdo&Shaklan1996.2000). adaptive-optics. and space-based. astrometry. using LST (Benedictetal.2002a). | This newly demonstrated approach to narrow-angle astrometry compares quite favorably with other astrometric methods used to date, such as speckle interferometry \citep{hor02,woi03}, single-telescope astrometry with \citep{l01} and without \citep{ps96,ps00}
adaptive-optics, and space-based astrometry using HST \citep{ben02}. |
. These have all produced measurement precisions on the order of 0.1-1 mas. | These have all produced measurement precisions on the order of 0.1-1 mas. |
The improved performance of (he interferometric approach is primarily due to the onger available baseline. | The improved performance of the interferometric approach is primarily due to the longer available baseline. |
However. the combination of phase-relerencing aud [ringe-scanning also compares lavorably to other interferometric methods. such as using fnnge visibility neasurements (o [find binary star orbits ( i.e. a Iractional precision of 10.1 as compared to 107. Boden οἱ al.. 2000)). | However, the combination of phase-referencing and fringe-scanning also compares favorably to other interferometric methods, such as using fringe visibility measurements to find binary star orbits ( i.e. a fractional precision of $10^{-4}$ as compared to $10^{-2}$, Boden et al., \nocite{boden00}) ). |
In this case the improvement comes from the unbiased nature of the phase estimator. | In this case the improvement comes from the unbiased nature of the phase estimator. |
Recent vears have seen a veritable explosion in (he number of known extrasolar planets (Schneider2003).. starting with (he famous example of 51 Pee (Alavor&Queloz1995). | Recent years have seen a veritable explosion in the number of known extra-solar planets \citep{Sch:03::}, starting with the famous example of 51 Peg \citep{May:95}. |
. To date. most of (hese svstenis have been found using high-precision radial velocity (echniques. alihough recent. photometric (ransit searches have observed several planets (Charbonneauetal.2000:IXonacki 2003). | To date, most of these systems have been found using high-precision radial velocity techniques, although recent photometric transit searches have observed several planets \citep{char00,kon03}. |
. ILowever. these methods have to a large extent avoiclec searching close (separation less than a lew arcseconds) binary stellar svstems. primarily because the techniques used are not well suited to such svstems. | However, these methods have to a large extent avoided searching close (separation less than a few arcseconds) binary stellar systems, primarily because the techniques used are not well suited to such systems. |
Therefore it is particularly interesting (o note that despite the deliberate avoidance of binaries. of (he more than 100 | Therefore it is particularly interesting to note that despite the deliberate avoidance of binaries, of the more than 100 |
The CMDs of the CLIVCs are quite dillerent from 2\LASS-based CMDs of the centres of the star-forming Lrregular companions of the Milky Was. the LMC and the SALC. | The CMDs of the CHVCs are quite different from 2MASS-based CMDs of the centres of the star-forming Irregular companions of the Milky Way, the LMC and the SMC. |
Fheir CAIDs. shown in Figure 9. exhibit the blue plume near .)-1. J-Ix« of zero. | Their CMDs, shown in Figure 9, exhibit the blue plume near J-H, $_S$ of zero. |
They. also show a well populated ROB. which urns into a luminous. extended AGB for J-H. J-Ix« colours arger than one. | They also show a well populated RGB, which turns into a luminous, extended AGB for J-H, $_S$ colours larger than one. |
The CAIDs of the CIIVCSs do not exhibit a due plume at colours similar to those seen in the Magellanic Clouds. | The CMDs of the CHVCs do not exhibit a blue plume at colours similar to those seen in the Magellanic Clouds. |
They. do not show AGB stars with colours similar o those seen in the MC's. | They do not show AGB stars with colours similar to those seen in the MCs. |
This rules out the presence of a voung stellar content in the CLIVCs with properties similar o those of Irregular galaxies of the Local Croup. | This rules out the presence of a young stellar content in the CHVCs with properties similar to those of Irregular galaxies of the Local Group. |
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