text stringlengths 128 2.05k |
|---|
Outer-orbit parameters (Table ) provide projected major axis as [MATH] = 1.456 [MATH] 0.019 AU. Neglecting small eccentricity of the orbit the maximum angular separation of the components is [MATH] Assuming [MATH] (Section ) the maximum angular separation is just about 13 mas. |
The full amplitude of the photocenter motion can be found assuming [MATH] and [MATH] = 1.09 and [MATH] = 13 mas as: [EQUATION] For VW LMi we get [MATH] = 5.0 mas. This is comparable to the typical residuals seen in the Hipparcos astrometric solutions. Some improvement of the astrometric solution can be obtained using p... |
Absolute parameters of the components Parameters of the components can be determined by a simple procedure used in Pribulla et al. ( 2006 . Using new determination of the inclination angle [MATH] = 79.0° and the projected total mass of the contact pair [MATH] , we obtain [MATH] |
The outer, 355-days orbit defines the mass ratio for the two pairs, [MATH] . Therefore, the true (not the projected) mass of the second spectroscopic binary is [MATH] . Using the projected mass [MATH] , we estimate the inclination of the orbit of the second pair to be about [MATH] . The outer, 355-day orbit is even les... |
[MATH] 0.07 M and the projected total mass of only 3.32 [MATH] 0.10 M , we obtain [MATH] = 64.1 [MATH] 4.2 [MATH] In the view of large uncertainties, the planes of the detached pair and mutual wide orbit could still be coplanar. |
Individual masses of components are then [MATH] = 1.66 M [MATH] = 0.70 M [MATH] = 1.11 M , and [MATH] = 1.09 M . Masses of the components are rather inconsistent with the fact that all four components show practically the same spectral type. Assuming [MATH] and that all four components produce energy as MS stars result... |
Conclusions Tightest known quadruple system VW LMi is really unique. It definitely deserves additional observations and analysis. The study of this system could bring light on (i) the evolution and origin of binary stars in multiple systems of stars (ii) tidal interaction of third body and its influence on the Roche ge... |
The study of VW LMi is, however, complicated by (i) the outer orbital period being close to one year which complicates its phase coverage by Earth-bound observer (ii) very small angular separation of the components making direct resolving of the mutual wide orbit and reliable determination of [MATH] difficult (which wo... |
It is also interesting to note, that VW LMi and HD95606 show very similar proper motion, parallax and RVs (see Table ) - the stars definitely form a loosely bound pair and all components very probably evolved from the same protostellar cloud (see Oswalt et al. ( 2007 ). |
The orbit of the detached pair in VW LMi with 7.93-days period is almost circular. This is the case of another two quadruples detected by the DDO observations, TZ Boo and V2610 Oph (DDO series No. XIV, Pribulla et al. ( 2008 ). That means that either it evolved with such orbit or it was circularized by the gravitationa... |
Better characterization of VW LMi calls for long-term monitoring to cover the whole 355-days orbital cycle. Especially, times of minima should be obtained free of any systematic effects. The understanding of the system would greatly benefit from visual orbit obtained by means of long-baseline interferometry. Multi-colo... |
The stays of TP at DDO have been supported by a grant to Slavek M. Rucinski from the Natural Sciences and Engineering Council of Canada. This research has been supported in part by the Slovak Academy of Sciences under grants No. 2/7010/7 and 2/7011/7, and grant of the Šafárik University VVGS 9/07-08. MV’s research is s... |
# Source: arxiv 0808.0132 # Title: GHASP : An Halpha kinematic survey of 203 spiral and irregular galaxies - VII. Revisiting the analysis of Halpha data cubes for 97 galaxies # Sections: all # Downloaded: 2026-03-02T07:58:55.678685+00:00 |
GHASP : An H [MATH] kinematic survey of 203 spiral and irregular galaxies - VII. Revisiting the analysis of H [MATH] data cubes for 97 galaxies. |
(Accepted. Received; in original form ) Abstract The GHASP survey (Gassendi HAlpha survey of SPirals) consists of 3D H [MATH] data cubes for 203 spiral and irregular galaxies, covering a large range in morphological types and absolute magnitudes, for kinematics analysis. It is the largest sample of Fabry-Perot data pub... |
keywords: Galaxies: spiral; irregular; dwarf; Galaxies: kinematics and dynamics; Introduction The GHASP survey consists of a large sample of spiral and irregular galaxies observed with a scanning Fabry-Perot for studying their kinematical and dynamical properties through the ionized hydrogen component. The goals of thi... |
(Garrido et al., 2002 2003 ; Garrido et al., 2004 ; Garrido et al., 2005 ; Spano et al., 2007 ; Epinat et al., 2008 presenting the data obtained in the frame of the GHASP survey. The observations were lead during fourteen observing runs at the “Observatoire de Haute Provence (OHP)”, France, from 1998 to 2004. The surve... |
To be clear on the goals and limits of this present work, we summarize hereafter what we present and what we do not in this paper. We present: |
the new individual maps and position-velocity diagrams in Appendix (on line data only), the new rotation curves, in Appendix and the new corresponding tables in Appendix |
In this paper, we lead the same kind of analysis as the one presented in Paper VI concerning: the study of the parameters of the kinematical models, |
the study of the residual velocity fields, the Tully-Fisher relation. Because it is useful to display and analyze all the data together, we put here in the same tables (in Appendix ) the new parameters and the results already published in Paper VI so that the reader does not have to compile tables coming from different... |
Because this has been discussed in previous papers, we do not present any more: the morphological types and luminosity distributions of the whole GHASP sample (see Paper VI), |
the data reduction procedure used here, including the computation of the rotation curves, the determination of the kinematical parameters and the determination of the uncertainties (see Paper VI), |
the instrumental set-up of the instrument for the data re-reduced in this paper (see Papers I to IV), the individual comments for each galaxy (see Papers I to IV), except when the new reduction procedure leads to new comments or to conclusions noticeably different from the previous ones (see Appendix ). |
In section we make an indirect flux calibration of the H [MATH] profiles. In section we present the data and in section we compute the Tully-Fisher relation. In section we give the summary and conclusions. When the distances of the galaxies are not known, a Hubble constant H =75 km s -1 Mpc -1 is used throughout this p... |
Calibration and H [MATH] profiles Even if direct flux calibration is always possible using well calibrated and extended H [MATH] emitters like planetary nebulae |
(Dopita & Hua, 1997 , during the observations, we decided not to calibrate our data, thus saving observing time. Indeed, our major scientific goal was not to use the Fabry-Perot technique to make photometric studies but kinematic ones. We estimated that H [MATH] flux calibrations require additional observing times rang... |
James et al. ( 2004 who do not separate H [MATH] from [NII] lines. We have corrected this effect assuming a mean and constant spectral ratio H [MATH] /[NII]=3. Distinct calibrations have been made depending on the observing setup. Indeed, the GHASP sample has been obtained using a 256 [MATH] 256 IPCS (Imaging Photon Co... |
James et al. ( 2004 fluxes and our estimated fluxes for the old IPCS (top) and the new IPCS (bottom). The linear regressions are plotted with the dashed lines and their coefficients are respectively 0.73 [MATH] 0.13 [MATH] and 0.48 [MATH] 0.06 |
[MATH] . The fluxes estimated from this calibration are presented in Table LABEL:table_calib Data Analysis As detailed in Paper VI, the same procedure (adaptive binning, sky subtraction, ghost removals, …) has been used to compute the data cubes and the maps deduced from these cubes. For each galaxy, in Appendix D (ava... |
LABEL:tabletf ) in order to compare the velocity field extent with the optical disk of the galaxies. Position-velocity diagrams are computed along the axis defined by this black line, using a virtual slit width of seven pixels. The red line superimposed on the position-velocity diagram is the rotation curve deduced fro... |
(figures) and (tables). They are computed and displayed following the method described in Paper VI. These figures are also available on the Fabry-Perot data base: |
. Appendix (that contains the tables corresponding to the rotation curves) is available online only. The curves are plotted with both sides superimposed in the same quadrant, using different symbols for the receding (crosses) and approaching (dots) side (with respect to the center). The black vertical arrow on the X-ax... |
while the smaller grey arrow on the X-axis represents the transition radius (defined in Paper VI), always smaller than [MATH] by definition. |
For galaxies seen almost edge-on (inclination higher than 75 ) our model does not describe accurately the rotation of a galaxy (see Paper VI). Furthermore, for UGC 1249, UGC 2082, UGC 3851, UGC 4278, UGC 5272, UGC 5935 and UGC 11909, neither rotation curve nor residual velocity fields have been plotted. For them, the p... |
The rotation curves recomputed in this paper may be different from the ones published in Papers I to V since: (i) the adaptive binning gives different weights to low signal-to-noise ratio regions in the velocity field from which is computed the rotation curve; (ii) the exclusion sector around the minor axis is always s... |
The mean velocity dispersion on each residual velocity field has been computed for each galaxy and tabulated in Table LABEL:tablemod Details on the computation and on the analysis of residual velocity fields are given in Paper VI. Taking into account the whole sample, the plot presented in Paper VI has been updated in ... |
The morphological parameters (input parameters of the fits) and the results of the fits (kinematical parameters, [MATH] , and parameters of the residual maps) are given in Table LABEL:tablemod Morphological types, distances, absolute magnitudes M , optical radii D [MATH] , axis ratios and references for HI velocity fie... |
and quality flag on V max ). The 25 galaxies larger than the field of view of the instrument are flagged in Col. 8 of Table LABEL:tabletf The galaxies for which it was necessary to decrease the degrees of freedom of the model have their fixed parameters flagged with an asterisk ( ) in Table LABEL:tablemod (see Paper VI... |
The kinematical position angles obtained by GHASP are compared with the photometric position angles (found in HyperLeda) and plotted in Figure |
. The error bar on the morphological position angle has been estimated using the axis ratio and optical radius uncertainties; for clarity, only one morphological position angle is plotted (see Paper VI). In Figure , we have used special symbols for galaxies with no accurate morphological position angle (red open circle... |
(bottom) indicates that (i) for 57% of the galaxies, the agreement is better than 10 ; (ii) for 79%, the agreement is better than 20 ; (iii) the disagreement is larger than 30 for 15% of the galaxies. The conclusion addressed in Paper VI remains valid, i.e. integral field spectroscopy constitutes the best technique to ... |
The kinematical and morphological inclinations are compared in Figure . On the top panel, the photometric inclination is computed using a correction factor depending on the morphological type (see Paper VI). On the middle panel the photometric inclination is derived from the axis ratio. Galaxies for which the morpholog... |
The Tully-Fisher relation Among the whole sample of 203 galaxies, we have plotted the Tully-Fisher relation ( Tully & Fisher, 1977 , M as a function of |
[MATH] ) for a sub-sample of 177 galaxies in Figure . The 26 other galaxies are not considered in the present discussion because (i) for seven galaxies the rotation curve does not reach the maximum rotation velocity (UGC 1117, UGC 1655, UGC 2455, UGC 4393, UGC 6523, UGC 8898 and UGC 9406); (ii) no B magnitude is availa... |
LABEL:tabletf ). The maximum velocity V max and its error have been obtained from the fit to the velocity field and the solid line in Figure |
is the relation found by Tully & Pierce ( 2000 (see Paper VI). In Figure (Top), the error bars on the velocity are displayed and galaxies with inclination lower than 25 are distinguished (blue open squares). As already noticed in Paper VI, these galaxies have statistically higher velocities than expected from the Tully... |
is reached for 76 of them (black dots, large size), probably reached for 44 of them (blue squares, medium size) and probably not reached for 35 of them (red triangles, small size). They are distinguished in Figure (Middle) and flagged in Table LABEL:tabletf The quality flag on the maximum velocity is given in Table |
LABEL:tabletf (see Paper VI). Figure (Middle) confirms the two classifications “V max probably reached” and“V max probably not reached” since for the majority of each class the points are respectively in agreement and above the |
Tully & Pierce ( 2000 relation. From the two classes “V max reached” and “V max probably reached”, we find the following relation (see Paper VI for additional details): |
[EQUATION] This relation is displayed as a dashed line in Figure , in which morphological types are distinguished for the two best classes (black circles from 0 to 2, red triangles from 2 to 4, blue squares from 4 to 6, green rhombuses from 6 to 8 and pink stars from 8 to 10). The slope of the linear regression compute... |
Tully & Pierce ( 2000 (this slope was found to be somewhat lower in Paper VI), and its uncertainty has been reduced by a factor 0.75. For the Tully-Fisher relation, we note that fast rotators (V [MATH] km s -1 : UGC 89, UGC 508, UGC 3429, UGC 4422, UGC 4820, UGC 5532, UGC 8900, UGC 8937, UGC 9969 and UGC 11470) are les... |
Summary and conclusions The knowledge of the links between the kinematical and dynamical state of galaxies helps us to increase our understanding of the physics and evolution of galaxies. The GHASP sample, which consists of 203 spiral and irregular galaxies, covering a wide range of morphological types and absolute mag... |
In this paper, 97 galaxies have been re-reduced using adaptive binning techniques in order to provide homogeneous data for the whole sample. For each galaxy, we have presented the H [MATH] velocity field, the [MATH] monochromatic image and eventually the H [MATH] residual velocity field, the position-velocity diagram a... |
From the data cubes, integrated H [MATH] profiles have also been produced. A post calibration has allowed to compute indirect absolute H [MATH] flux for all the galaxies belonging to the GHASP sample. This post calibration has been done using fluxes for 69 galaxies found in the literature (James et al., 2004 |
We confirm and strengthen most of the results already obtained from half the sample: A high quality model has been achieved to represent the axi-symmetric rotational component of the galaxies since no typical signatures for biases are observed in the residual velocity fields. This means that the residuals observed in t... |
The mean residual velocity dispersion is strongly correlated with the maximum amplitude of the velocity field. For a given velocity range, this correlation does not clearly depend on the morphological type. However strongly barred galaxies have a higher residual velocity dispersion than mild-barred or unbarred galaxies... |
The determinations of kinematical position angles are robust whatever the inclination of the galaxy whereas morphological position angles are poorly determined for low inclination systems. Moreover, morphological position angles have systematically higher uncertainties than kinematical ones. This is a major argument fo... |
Galaxies with poor determination of their morphological position angles have usually unreliable and overestimated morphological inclinations. The agreement between kinematical and morphological inclinations is better when assuming a thin disk in particular for high inclination galaxies. For galaxies with intermediate d... |
The use of the whole GHASP sample leads to a Tully-Fisher relationship in perfect agreement with Tully & Pierce ( 2000 , despite important differences in the selection of both samples. With respect to the result presented in Paper VI, the use of the whole sample increases the agreement with |
Tully & Pierce ( 2000 . Three comments should be underlined: (i) galaxies with inclination lower than 25 are inappropriate for Tully-Fisher relation determination since their estimated velocities are easily overestimated; (ii) fast rotators (V [MATH] 300 km s -1 ) are maybe less luminous (than expected from the Tully-F... |
From these data and analysis, it is now possible to adress the scientific drivers on the whole GHASP sample in forthcoming papers. |
acknowledgements The authors warmly thank their collaborators: Philippe Balard, Chantal Balkowski, Jacques Boulesteix, Olivier Boissin, Claude Carignan, Laurent Chemin, Olivier Daigle, Jean-Luc Gach, Olivia Garrido and Olivier Hernandez for having participated to the previous works making possible the new analyze of th... |
). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present ... |
Appendix A Notes on individual galaxies UGC 508 . HI inclination (25 Noordermeer et al., 2005 ) as well as photometric inclination (14 , from an axis ratio of 0.97) lead to a very high maximum rotation velocity [MATH] 550 km s -1 ). From Tully-Fisher relationship, its absolute magnitude suggests a maximum velocity arou... |
UGC 1117 . This galaxy is the famous M33. Because of the limited field-of-view of GHASP we only observed the solid body central part of the rotation curve. The external round shape structures in the different images are due to edge-effects of the interference filter vignetting the field-of-view. |
UGC 1249 . No rotation curve has been computed because of its high inclination (90 ). UGC 1256 . Within [MATH] 25″ ( [MATH] 1 kpc), the rotation curve shows negative rotation velocity. This is due to the fact that the bar is almost parallel to the major axis. |
UGC 1736 . The kinematical center chosen in Paper IV is different from the morphological center chosen here, leading to a different rotation curve. |
UGC 1913 . Same comment as for UGC 1736. UGC 2023 . Despite the fact that this galaxy has been observed again (2 hours exposure time on September 11th 2002) and that these data have been compared and added to the data presented in Paper II, the signal-to-noise ratio remains very weak. From the R-band image observed by ... |
Swaters ( 1999 . The kinematical center chosen in Paper II is quite different from the one used here (13″ westward now, which is 0.5 kpc), leading to a very different shape for the rotation curve. Despite the fact that the systemic velocities are almost the same, in Paper II the rotation curve reaches a plateau at [MAT... |
UGC 2034 . Despite the fact that this galaxy has been observed again for 1.5 hours (on September 12th 2002) and that these data have been compared and added to the data presented in Paper II, the signal-to-noise ratio remains very weak. Due to the lack of rotation and of spatial coverage, our model does not converge. T... |
UGC 2045 . A difference of 6 is computed between the major axis position angle given in this paper and in Paper IV. This is due to the warp which biases the automatic determination of the major axis position angle with respect to the morphological one. It leads to little change however in the rotation curve. The maximu... |
UGC 2053 . The signal-to-noise ratio and the total H [MATH] flux of this galaxy are very low. The new maps are not much different from the ones published in Paper II, so that they are not presented here. |
UGC 2080 . The determination of the inclination of this almost face-on galaxy leads to lower value when using the kinematics than when using the morphology. A too low inclination leads to a maximum rotation velocity too high with respect to its magnitude and its optical radius. The distance of this nearby galaxy is not... |
UGC 2082 . Using the rule defined in Paper VI, we have not plotted the rotation curve of this edge-on galaxy. The maximum rotation velocity may be not reached. |
UGC 2141 . The signature of a strong bar is clearly visible in the velocity field. It is almost aligned with the major axis and may explain the difference between the value of major axis position angle found in this study and that published in Paper IV (7 ). The major axis position angle probably changes with radius wi... |
UGC 2183 . The inclination computed here (41 [MATH] 10 ) is similar to the morphological one (47 ) but quite different from that found in HI by |
Swaters ( 1999 and adopted in Paper IV (62 ). The value 90 suggested by Noordermeer et al. ( 2005 from optical measurements does not seem realistic. |
UGC 2455 . The velocity field of this faint low surface brightness galaxy shows a small amplitude making difficult the determination of the rotation curve which is, moreover, affected by a strong bar. |
UGC 3013 . The determination of the morphological position angle is biased by a strong bar and spiral arms. UGC 3382 . This galaxy has been published in Paper VI from data coming only from run 13. Nevertheless, this galaxy was already observed in run 5 but never published because the signal-to-noise ratio was too low. ... |
UGC 3429 . The nucleus of the galaxy is probably hidden behind a dust lane, so that its true position is hard to find on the continuum images because of strong absorption. Thus, we use the center making the central part of the rotation curve most symmetric. This leads to a satisfactory position for the rotation center ... |
(Marcum et al., 2001 UGC 3574 . With respect to Paper I, the inclination has been reduced from 30 to 19 [MATH] 10 , this new value is more compatible with the morphological one (21 ) but leads to a very high maximum rotation velocity with respect to its faint absolute magnitude (M =-18.0, James et al., 2004 ). For this... |
UGC 3851 . The ghost on the data (located on the northern side of the image) has been removed. No rotation curve has been computed because of its high inclination and to the fact that the velocity field corresponding to the very bright region south of the galaxy may be an artefact due to the detector. |
UGC 4273 . The determination of the morphological position angle is biased by the bar and spiral arms. UGC 4278 . No rotation curve has been computed because of its high inclination (90 ). |
UGC 4284 . The rotation curve is more symmetrical using a kinematical center 5″ south from the morphological center. However, to have a consistent analysis with the rest of the sample, we decided to keep the morphological center. |
UGC 4305 . The center has been changed from Paper III, and is now more to the East. It has been determined from a 2MASS image in the infrared. This center still gives a fairly symmetric rotation curve. It coincides approximately with the HI kinematical center but absolutely not with the optical center of isophotes. The... |
UGC 4499 . The inclination has been set to the value computed by Swaters et al. ( 2003 UGC 4543 . The morphological position angle of this galaxy is difficult to estimate due to its “Magellanic” structure. |
UGC 4936 . The inclination found now is 17 lower than the one published in Paper III. This value is more compatible with the absolute magnitude of the galaxy as well as its optical radius. |
UGC 5272 . The position-velocity diagram displays a solid body structure characteristic of a bar like structure or an edge-on galaxy. The optical and H [MATH] images both look like a bar rather than a disk galaxy, suggesting a morphological inclination close to 90 . Thus no rotation curve has been plotted. The HI incli... |
UGC 5721 . The uncommon rotation curve results from the very irregular velocity field perturbed by a strong bar. UGC 5931 . The morphological position angle of this galaxy is difficult to estimate due to the interaction with its close companion UGC 5935. |
UGC 5935 . No rotation curve has been computed because of its high inclination, close to 90 UGC 6537 . The rotation center has been assumed to be the strong nucleus, leading to an asymmetric rotation curve in the outer regions, compatible with the asymmetric velocity field. In Paper III, in order to get a symmetric rot... |
UGC 7278 . This galaxy does not show any evidence for rotation. However, a velocity amplitude of about 10 km s -1 is observed on its velocity field. |
UGC 7524 . The velocity field only covers the bar of the galaxy which is almost aligned with the HI major axis position angle, thus no rotation curve has been plotted. Furthermore, only the central part of this galaxy is seen in our field-of-view. |
UGC 7592 . This galaxy does not show any evidence for rotation. However, a velocity amplitude of about 25 km s -1 is observed on its velocity field. |
UGC 10310 . The morphological position angle is difficult to estimate due to the nature of this barred Magellanic galaxy. UGC 10359 . The determination of the morphological position angle is biased by a strong bar and spiral arms. |
UGC 10445 . The presence of a bar and spiral arms make both morphological and kinematical position angles determinations difficult. |
UGC 10470 . A strong bar in this galaxy biases the determination of the major axis position angle and of the inclination. For the latter we adopted the value suggested by the morphological axis ratio (34 from the NED). |
UGC 10502 . The kinematical inclination is much higher than the morphological one (24 from the axis ratio). Since this galaxy is interacting, its morphological inclination may be underestimated because of its open spiral arms distorted by streaming motions. The average morphological inclination given in Hyperleda is in... |
UGC 10897 . The morphological position angle is poorly determined for this low inclination galaxy. UGC 11124 . The inclination is difficult to determine because of a strong bar in this interacting galaxy. The kinematical inclination (51 ) is higher than the morphological one determined from the axis ratio (22 ). Despit... |
UGC 11283 . The presence of a strong bar and spiral arms make both morphological and kinematical position angle determinations difficult. |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.