AMIGA : Star formation

Isolated Galaxies - Infrared Diagnostics - Hα study of a redshift-limited subsample - Star formation in bars - Star formation in outer disks -

Isolated Galaxies - Infrared Diagnostics - Hα study of a redshift-limited subsample - Star formation in bars - Star formation in outer disks - Optical colors of isolated galaxies Compact Groups - Strong far-infrared cooling lines, peculiar CO kinematics, and possible star-formation suppression in Hickson Compact Group 57 - Star formation suppression in compact group galaxies: a new path to quenching? Star formation in bars As explained in "Hα study of a redshift-limited subsample", one of the aspects of our project was to study the Hα emission of isolated spirals in its different aspects. Star formation depends strongly both on the local environment of galaxies, and on the internal dynamics of the interstellar medium. To disentangle the two effects, we obtained, in the framework of the AMIGA project, Hα and Gunn r photometric data for more than 200 spiral galaxies lying in very low-density regions of the local Universe. In one of our studies we caracterise Hα emission, tracing current star formation, of the 45 largest and less inclined galaxies observed for which we estimate the torques between the gas and the bulk of the optical matter. We could subsequently study the Hα morphological aspect of these isolated spiral galaxies. The imposed requirements have been: Major axis a ≥ 1' to have a sufficient spatial resolution Inclination i ≤ 50° in order to obtain a sufficiently accurate deprojection. Image analysis In order to calculate the gravitational potential, density and torques in the plane of the disks of the galaxies, we processed the Hα and Gunn r corrected images as follows: the r band image (not scaled to Hα) and the Hα continuum subtracted image were used. The Gunn r images were used in order to estimate the gravitational potential of the galaxies. To determine the bar/arm force at each radius, we made use of the method developed by García-Burillo et al. (1993, 2005) to compute the gravitational potential, applying it to our red images, supposing a constant stellar mass-to-light (M/L) ratio. A Fourier-component analysis of the potential was performed, using the m = 2 component to get the tangential forces (Block et al. 2002) and the m = 0 component to get the axisymmetric forces. Their quotient gives us a measurement of the bar/arm force. We estimated the average torque depending on the radius: using the gravitational forces and the young stars born from the gas (Hα), we obtained the phase shift between gaseous arms and the potential well which creates the torques. Generally, due to the bar gravity torques, the gas flows into the centre (negative torque) from the corotation radius to the inner Linblad resonance (ILR) and flows outwards (positive torque) when outside the corotation radius, until the outer Lindblad resonance (OLR). This can be effectively observed for the galaxies in our sample. Finally, we estimated the angular momentum transfer and therefore the evolution time for bars in isolated galaxies. Fig. 1 Fig. 2 As an example, Figs. 1 & 2 display the images and graphics of the potential, density and torques corresponding to CIG 30 & CIG 1004, respectively. The first row shows the Gunn r broadband filter (left) and Hα narrow-band filter (right) deprojected images, from which the potential, density and torques have been estimated. The second row corresponds to the amplitude (left) and the phase (right) of the Fourier components of the potential. The third row corresponds to the amplitude (left) and phase (right) of the Fourier components of the density. For the graphics of the potential and the density, the legend is the following: dashed line represents m = 1; full line represents the m = 2 component (and the sum also for the amplitude of the potential as it is always above and cannot be confused with the others); dot-dash-dot-dash represents m = 3; dotted line represents m = 4. The torques as a function of the radius of the galaxy is presented in the bottom left panel. The corotation occurs at the radius defined by the change of sign for dL/L. And dL/L shows that in one rotation, the gas loses a non negligible fraction of its angular momentum, which can bring constraints on the life time of the morphological patterns of the galaxy. The legend in the bottom right corner gathers the CIG number, the observed recession velocity (in km s−1), the optical diameter D25 (in ´), the blue luminosity, the morphological type and the group to which the galaxy belongs. The Gunn r and Hα images, along with the graphics of the potential, density and torques of the full sample of the 45 galaxies are available in Verley et al. 2007 Conclusions We performed a detailed morphological study of this sample and compared it with numerical simulations, coming to the following results: The percentage of bars (60% in the optical) shows that isolated galaxies are not preferentially barred or unbarred galaxies. The histogram of relative tangential force strengths is quite similar to other samples of galaxies selected without regard to any isolation criterion. Frequently, we observed a phase shift between gas and stellar components: the Hα emission is always leading with respect to the bar in the Gunn r image (shift angle ~ 10°). We interpreted the various global Hα morphologies observed in terms of the secular evolution experienced by galaxies in isolation. The main Hα classes can be related to the bar evolution phases. The observed frequency of particular patterns brings constraints on the time spent in the various evolution phases. We chose to group the galaxies presenting similar features, we defined three main groups: group E (19 galaxies) gathers the galaxies showing a strong central peak in the Hα emission, Hα emission along the spiral arms but not in the bar. Group F (9 galaxies) is constituted by galaxies with less gas, which do not present any central emission knot in Hα. Galaxies in group G (8 galaxies) show Hα emission in the bar. Other groups with fewer galaxies were also defined, most noticeable is the group EG (3 galaxies) featuring galaxies having characteristics in between those defined by the groups E andG. Hence, we could interpret these features as different stages of an evolutive sequence: G -> EG -> E -> F. Numerical simulations showed a predicted frequency of the G phase higher than the E phase, in contradiction with our observations.We attribute this discrepancy to a failure of the star formation recipe, since we used the usual local Schmidt law for the star formation rate. The frequently observed phenomenon of star formation avoiding the bar, in spite of large gas density there, suggests that the star formation law should depend also on other factors, in particular the relative velocity of the gas in the bar. Verley et al. 2007
 

Star formation

Isolated Galaxies
- Infrared Diagnostics
- Hα study of a redshift-limited subsample
- Star formation in bars
- Star formation in outer disks
- Optical colors of isolated galaxies
Compact Groups
- Strong far-infrared cooling lines, peculiar CO kinematics, and possible star-formation suppression in Hickson Compact Group 57
- Star formation suppression in compact group galaxies: a new path to quenching?

Star formation in bars

As explained in "Hα study of a redshift-limited subsample", one of the aspects of our project was to study the Hα emission of isolated spirals in its different aspects. Star formation depends strongly both on the local environment of galaxies, and on the internal dynamics of the interstellar medium. To disentangle the two effects, we obtained, in the framework of the AMIGA project, Hα and Gunn r photometric data for more than 200 spiral galaxies lying in very low-density regions of the local Universe. In one of our studies we caracterise Hα emission, tracing current star formation, of the 45 largest and less inclined galaxies observed for which we estimate the torques between the gas and the bulk of the optical matter. We could subsequently study the Hα morphological aspect of these isolated spiral galaxies. 

The imposed requirements have been:

  • Major axis a ≥ 1' to have a sufficient spatial resolution
  • Inclination i ≤ 50° in order to obtain a sufficiently accurate deprojection.

Image analysis
In order to calculate the gravitational potential, density and torques in the plane of the disks of the galaxies, we processed the Hα and Gunn r corrected images as follows: the r band image (not scaled to Hα) and the Hα continuum subtracted image were used. The Gunn r images were used in order to estimate the gravitational potential of the galaxies.

To determine the bar/arm force at each radius, we made use of the method developed by García-Burillo et al. (1993, 2005) to compute the gravitational potential, applying it to our red images, supposing a constant stellar mass-to-light (M/L) ratio. A Fourier-component analysis of the potential was performed, using the m = 2 component to get the tangential forces (Block et al. 2002) and the m = 0 component to get the axisymmetric forces. Their quotient gives us a measurement of the bar/arm force.

We estimated the average torque depending on the radius: using the gravitational forces and the young stars born from the gas (Hα), we obtained the phase shift between gaseous arms and the potential well which creates the torques. Generally, due to the bar gravity torques, the gas flows into the centre (negative torque) from the corotation radius to the inner Linblad resonance (ILR) and flows outwards (positive torque) when outside the corotation radius, until the outer Lindblad resonance (OLR). This can be effectively observed for the galaxies in our sample. Finally, we estimated the angular momentum transfer and therefore the evolution time for bars in isolated galaxies.
 

IC35 Star formation in isolated AMIGA galaxies
Fig. 1		 NGC 7479 Star formation in isolated AMIGA igalaxies
Fig. 2

As an example, Figs. 1 & 2 display the images and graphics of the potential, density and torques corresponding to CIG 30 & CIG 1004, respectively. The first row shows the Gunn r broadband filter (left) and Hα narrow-band filter (right) deprojected images, from which the potential, density and torques have been estimated. The second row corresponds to the amplitude (left) and the phase (right) of the Fourier components of the potential. The third row corresponds to the amplitude (left) and phase (right) of the Fourier components of the density. For the graphics of the potential and the density, the legend is the following: dashed line represents m = 1; full line represents the m = 2 component (and the sum also for the amplitude of the potential as it is always above and cannot be confused with the others); dot-dash-dot-dash represents m = 3; dotted line represents m = 4. The torques as a function of the radius of the galaxy is presented in the bottom left panel. The corotation occurs at the radius defined by the change of sign for dL/L. And dL/L shows that in one rotation, the gas loses a non negligible fraction of its angular momentum, which can bring constraints on the life time of the morphological patterns of the galaxy. The legend in the bottom right corner gathers the CIG number, the observed recession velocity (in km s−1), the optical diameter D25 (in ´), the blue luminosity, the morphological type and the group to which the galaxy belongs. The Gunn r and Hα images, along with the graphics of the potential, density and torques of the full sample of the 45 galaxies are available in PDF File Verley et al. 2007

Conclusions
We performed a detailed morphological study of this sample and compared it with numerical simulations, coming to the following results:

  • The percentage of bars (60% in the optical) shows that isolated galaxies are not preferentially barred or unbarred galaxies. The histogram of relative tangential force strengths is quite similar to other samples of galaxies selected without regard to any isolation criterion.
  • Frequently, we observed a phase shift between gas and stellar components: the Hα emission is always leading with respect to the bar in the Gunn r image (shift angle ~ 10°).
  • We interpreted the various global Hα morphologies observed in terms of the secular evolution experienced by galaxies in isolation. The main Hα classes can be related to the bar evolution phases. The observed frequency of particular patterns brings constraints on the time spent in the various evolution phases.
  • We chose to group the galaxies presenting similar features, we defined three main groups: group E (19 galaxies) gathers the galaxies showing a strong central peak in the Hα emission, Hα emission along the spiral arms but not in the bar. Group F (9 galaxies) is constituted by galaxies with less gas, which do not present any central emission knot in Hα. Galaxies in group G (8 galaxies) show Hα emission in the bar.
  • Other groups with fewer galaxies were also defined, most noticeable is the group EG (3 galaxies) featuring galaxies having characteristics in between those defined by the groups E andG. Hence, we could interpret these features as different stages of an evolutive sequence: G -> EG -> E -> F.
  • Numerical simulations showed a predicted frequency of the G phase higher than the E phase, in contradiction with our observations.We attribute this discrepancy to a failure of the star formation recipe, since we used the usual local Schmidt law for the star formation rate. The frequently observed phenomenon of star formation avoiding the bar, in spite of large gas density there, suggests that the star formation law should depend also on other factors, in particular the relative velocity of the gas in the bar.

PDF File Verley et al. 2007