Molecular gas and star formation in the Tidal Dwarf
Galaxy VCC 2062

U., Lisenfeld, J. Braine, P.A. Duc, M., Boquien, E., Brinks, F., Bournaud, F., Lelli, V., Charmandaris

► To cite this version:

U., Lisenfeld, J. Braine, P.A. Duc, M., Boquien, E., Brinks, et al.. Molecular gas and star formation in the Tidal Dwarf Galaxy VCC 2062. Astronomy & Astrophysics - A&A, 2016, 590, pp.id.A92. 10.1051/0004-6361/201527887 . hal-01302311

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<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
Molecular gas and star formation in the tidal
dwarf galaxy VCC 2062*

U. Lisenfeld<fnref n="1" />, J. Braine<fnref n="2" />, P. A. Duc<fnref n="3" />, M. Boquien<fnref n="4" />,<fnref n="5" />, E. Brinks<fnref n="6" />, F. Bournaud<fnref n="3" />, F. Lelli<fnref n="7" />, and V. Charmandaris<fnref n="8" />,<fnref n="9" />

Received 3 December 2015 / Accepted 29 March 2016

ABSTRACT

The physical mechanisms driving star formation (SF) in galaxies are still not fully understood. Tidal dwarf galaxies (TDGs), made of gas ejected during galaxy interactions, seem to be devoid of dark matter and have a near-solar metallicity. The latter makes it possible to study molecular gas and its link to SF using standard tracers (CO, dust) in a peculiar environment. We present a detailed study of a nearby TDG in the Virgo Cluster, VCC 2062, using new high-resolution CO(1–0) data from the Plateau de Bure, deep optical imaging from the Next Generation Virgo Cluster Survey (NGVS), and complementary multiwavelength data. Until now, there was some doubt whether VCC 2062 was a true TDG, but the new deep optical images from the NGVS reveal a stellar bridge between VCC 2062 and its parent galaxy, NGC 4694, which is clear proof of its tidal origin. Several high-resolution tracers ($H\alpha$, UV, 8 µm, and 24 µm) of the star formation rate (SFR) are compared to the molecular gas distribution as traced by the CO(1–0). Coupled with the SFR tracers, the NGVS data are used with the CIGALE code to model the stellar populations throughout VCC 2062, yielding a declining SFR in the recent past, consistent with the low $H\alpha$/UV ratio, and a high burst strength. HI emission covers VCC 2062, whereas the CO is concentrated near the HI maxima. The CO peaks correspond to two very distinct regions: one with moderate SF to the NE and one with only slightly weaker CO emission but with nearly no SF. Even where SF is clearly present, the SFR is below the value expected from the surface density of the molecular and the total gas as compared to spiral galaxies and other TDGs. After discussing different possible explanations, we conclude that the low surface brightness is a crucial parameter to understand the low SFR.

**Key words.** ISM: molecules – galaxies: interactions – galaxies: ISM – galaxies: star formation – galaxies: dwarf

**1. Introduction**

Tidal dwarf galaxies (TDGs) are self-gravitating entities formed
from the tidal debris of interacting galaxies (see Duc 2012, and
references therein). Their stellar and star formation (SF) prop-
erties are similar to those of dwarf irregulars or blue compact
dwarfs, with the noticeable exception that their metallicity is
higher (about 1/3 solar to 1/2 solar) because they are recycled
objects, inheriting the metallicity of the outer regions of their
parent galaxies. Another relevant difference compared to non-
tidal dwarfs (called “classical” dwarf galaxies in the follow-
ing) is their expected lack of non-baryonic dark matter (DM)
if the standard Lambda cold dark matter (ACDM) cosmological
scenario is correct and DM is distributed in a large, pressure-
supported halo. Since a typical tidal interaction between two
galaxies mostly expels material from the disk, it is predicted
that only a fraction of DM resides in TDGs. This characteristic

is the strongest difference between TDGs and classical dwarfs,
but it is difficult to test because the dynamical and the visible
masses both need to be measured (see Duc 2012, for a review).
A rough estimate of the dynamical mass from the CO(1-0)
linewidth gave a low dark-to-visible mass ratio of the order
~1 in 8 TDGs (Braine et al. 2001), considerably lower than
the value typically found in classical dwarfs (baryon fraction
of ~30%, e.g. Lelli et al. 2014). In order to better determine
the dynamical mass, high-quality, high-resolution spectral data
are necessary to spatially resolve the gas kinematics. This has
been done, so far, in three systems based on high-resolution HI
data: NGC 5291, containing three TDGs (Bournaud et al. 2007,
revised in Lelli et al. 2015); NGC 7252 containing two ob-
jects (Lelli et al. 2015); and VCC 2062 (Lelli et al. 2015). In all
six TDGs, assuming dynamical equilibrium, the dark-to-visible
mass ratio is consistent with 1 giving strong support to the tidal
origin of the objects.

A major challenge in astrophysics is understanding the pro-
cess of SF in galaxies and in particular how the star forma-
tion rate (SFR) is quantitatively related to the neutral gas (the

<footnote n="1">¹ Departamento de Física Teórica y del Cosmos, Universidad de Granada, Spain and Instituto Carlos I de Física Téorica y Computacional, Facultad de Ciencias, 18071 Granada, Spain
e-mail: ute@ugr.es</footnote>

<footnote n="2">² Observatoire de Bordeaux, UMR 5804, CNRS/INSU, BP 89, 33270 Floirac, France</footnote>

<footnote n="3">³ Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot, DAPNIA/Service d'Astrophysique, CEA-Saclay,
91191 Gif-sur-Yvette Cedex, France</footnote>

<footnote n="4">⁴ Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK</footnote>

<footnote n="5">⁵ Unidad de Astronomía, Fac. Cs. Básicas, Universidad de Antofagasta, Avda. U. de Antofagasta 02800, Antofagasta, Chile</footnote>

<footnote n="6">⁶ Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK</footnote>

<footnote n="7">⁷ Astronomy Department, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106, USA</footnote>

<footnote n="8">⁸ Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, 15236 Penteli, Greece</footnote>

<footnote n="9">⁹ University of Crete, Department of Physics, 71003 Heraklion, Greece</footnote>

<footnote>* The reduced data cubes are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/590/A92</footnote>
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Optical false-colour image based on a combination of *u*, *g* and *i*-bands from the NGVS of the system NGC 4694 and VCC 2062. In blue the HI emission is overlaid. At the bottom, enlarged images of 3 regions within the HI tail are shown: the TDG VCC 2062, and two small SF regions at the end of the HI tail, HII-a and HII-b.</figcaption></figure>

with a central position of RA 12:48:00.2, Dec 10:58:10 and off-
sets of (5", 6") and (-14", 7"). We observed the CO(1-0) line at a central sky-frequency of 114.842 GHz corresponding to a recession velocity of 1120 km s⁻¹. The November data suffered from cable phase inversion on antennas 5 and 6. The data were corrected a posteri for this problem. The observations were car-
ried out under good weather conditions. 3C 273 was used as a phase and flux calibrator. We used the correlator in two settings, one providing a velocity resolution of 0.82 km s⁻¹ and a band-
width of 203 km s⁻¹, and the other at a velocity resolution of 6.2 km s⁻¹ and a bandwidth of 2130 km s⁻¹. The data with the lower resolution and larger bandwidth were used to search for emission at high velocity offsets and as an attempt to detect the continuum emission. We did not find emission outside the veloc-
ity range explored with high-resolution data and neither did we

detect any continuum emission. In the following we focus our
analysis on the high-velocity resolution data.

We reduced the data following standard procedures using the GILDAS<fnref n="3" /> software. Since the emission in our maps was rather weak, we used natural weighting to maximize the sensitivity. The untapered map achieved an angular resolution of 3′′2 × 2′′4 but showed only weak emission. We therefore applied different tapers to the data producing maps at different angular resolutions (4′′3 × 4′′1 for a taper to 90 m and 7′′7 × 6′′3 for a taper to 50 m). We will call these datacubes taper50 and taper90 in the following. We used the Högbom cleaning procedure, and tried also the Clark procedure which gave no important differences. In the cleaning process we identified and marked in each channel

<footnote n="3">³ http://www.iram.fr/IRAMFR/GILDAS</footnote>
<table><caption>**Table 1.** Summary of the observations used in this study.</caption><thead><tr><th>Telescope</th><th>Instrument/ Filter</th><th>λ<sub>0</sub>/ν<sub>0</sub></th><th>FWHM ["]</th><th>Δ<sub>cal</sub><sup>a</sup> [%]</th></tr></thead><tbody><tr><td>GALEX</td><td>FUX</td><td>0.154 µm</td><td>4.2</td><td>4.7</td></tr><tr><td>GALEX</td><td>NUV</td><td>0.232 µm</td><td>5.3</td><td>2.8</td></tr><tr><td>NGVS</td><td><i>u</i></td><td>0.381 µm</td><td>1</td><td>4.7</td></tr><tr><td>NGVS</td><td><i>g</i></td><td>0.487 µm</td><td>1</td><td>4.7</td></tr><tr><td>NGVS</td><td><i>i</i></td><td>0.769 µm</td><td>0.6</td><td>4.7</td></tr><tr><td>NGVS</td><td><i>z</i></td><td>0.887 µm</td><td>1</td><td>9.6</td></tr><tr><td><i>Spitzer</i></td><td>IRAC</td><td>3.5 µm</td><td>1.6</td><td>10</td></tr><tr><td><i>Spitzer</i></td><td>IRAC</td><td>4.5 µm</td><td>1.7</td><td>10</td></tr><tr><td><i>Spitzer</i></td><td>IRAC</td><td>5.8 µm</td><td>1.9</td><td>10</td></tr><tr><td><i>Spitzer</i></td><td>IRAC</td><td>8.0 µm</td><td>2.0</td><td>10</td></tr><tr><td><i>Spitzer</i></td><td>MIPS</td><td>24 µm</td><td>6</td><td>10</td></tr><tr><td>PdBI</td><td><sup>12</sup>CO(1–0)</td><td>114.8 GHz</td><td>4.3 × 4.1<sup>b</sup></td><td>–</td></tr><tr><td>VLA</td><td>HI</td><td>1.45 GHz</td><td>14.7 × 14.3</td><td>–</td></tr></tbody></table>

Notes. (a) The calibration uncertainties are from Morrissey et al. (2007; GALEX), Raichoor et al. (2011; NGVS), Fazio et al. (2004; IRAC) and Rieke et al. (2004), Engelbracht et al. (2007), Verley et al. (2009; MIPS). We do not include calibration errors in the CO and HI data. (b) Beam FWHM of the taper90 datacube.

the areas containing emission. We used a loop gain of 0.1 (we also tried a loop gain of 0.2 without noticing important differences). We cleaned down to 1.5% of the peak emission (which corresponds to about 0.5σ). We used the recommended truncation threshold of 0.2 of the primary beam sensitivity. We binned 2 channels of the high-velocity resolution data yielding a velocity resolution of 1.6 km s⁻¹.

## 2.2. Multiwavelength data from Duc et al. (2007)

We made use of the large collection of data presented in Duc et al. (2007), in particular single-dish CO(1–0) and CO(2–1) data from the IRAM 30 m telescope, HI data, UV data in the FUV (λ = 154 nm) and NUV (λ = 232 nm) band from GALEX and an Hα map. A detailed description of these observations and their data reduction are presented in Duc et al. (2007). Here we only summarise the most relevant aspects.

The HI data were retrieved from the VLA archive. They had originally been obtained as part of the VIVA project (project ID: AK563), a systematic survey of HI rich objects in VIRGO (Chung et al. 2009). The final, robustly weighted HI data cube that we use here has a beam of 14′′7 × 14′′3 and an rms noise of 0.6 mJy beam⁻¹, corresponding to a detection threshold (assuming a 3σ detection across 3 channels) of 9 × 10¹⁹ cm⁻². The velocity resolution is 7.3 km s⁻¹.

The CO spectra were observed with the IRAM 30 m telescope. A map with a spacing between pointings of 7′′ was obtained, covering roughly the extent of the HI cloud (see Fig. 2 of Duc et al. 2007). The velocity resolution is 2.6 km s⁻¹ for the CO(1–0) spectra and 1.3 km s⁻¹ for CO(2–1).

## 2.3. Spitzer data

We downloaded data obtained with the *Spitzer* telescope (Werner et al. 2004) from the *Spitzer* Heritage Archive. The field containing VCC 2062 was observed with the Infrared Array Camera (IRAC, Fazio et al. 2004) and with the Multiband

<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Deep g-band image from the NGVS of NGC 4694 and VCC 2062.</figcaption></figure>

Imaging Photometer (MIPS, Rieke et al. 2004). The images were processed with the *Spitzer* Super-Mosaic Pipeline and no further reduction was carried out. VCC 2062 was detected in all IRAC bands and in the 24 µm MIPS band. It was not detected by MIPS at 70 µm nor 160 µm.

## 2.4. Deep optical data

The deep optical images used in this paper were obtained at the Canada-France-Hawaii Telescope as part of the Next Generation Virgo Cluster Survey (NGVS, Ferrarese et al. 2012). NGVS used an observing strategy and data reduction pipeline (ELIXIR-LSB, Cuillandre et al., in prep.; Duc et al. 2015) optimized for the detection of extended LSB objects. Images were obtained in the *u*, *g*, *i*, and *z*-bands. Thanks to the low limiting surface brightness achieved – about 29 mag arcsec⁻² in the *g*-band –, a wealth of so far unknown faint stellar structures could be detected around NGC 4694 and give new insight in the history of this galaxy and its relation to VCC 2062.

Figure 1 shows a combined three-colour image of both objects in which the SF regions in VCC 2062 are clearly visible. Both galaxies are connected by a long and broad HI plume which extends to about twice the distance between them. Interestingly, towards the end of this HI plume, two further, much smaller, SF regions can be seen.

Figure 2 shows an image in the *g*-band, in which the low brightness structures are highlighted. The distorted and asymmetric appearance of NGC 4694 can be seen. Very noticeable is the broad stellar bridge from this galaxy to VCC 2062.

# 3. Properties of the molecular gas

## 3.1. Distribution and mass of the molecular gas

Appendix A presents the channel maps of the taper50 data cube showing that emission is visible in the velocity range between 1129 and 1159 km s⁻¹, distributed in various clouds and showing a velocity gradient along the NE–SW direction. In Fig. 3 we display the velocity integrated CO map. In the upper panel, two clearly separated regions of emission are visible which we call the NE and the SW clouds. In the very South, close to the edge of our imaged area, there is a further region (labelled “Southern cloud”). We tested the significance of this emission by creating
<figure><img src="image_4.png" /><figcaption>Fig. 3. Velocity integrated (from 1129 to 1159 km s⁻¹) intensity of the CO(1–0) data cube. Different regions of emission are labelled. The contours indicate the apertures used to derive the fluxes. Upper panel: data cube tapered at 50m (beam size 7''7 × 6''3), lower panel: data cube tapered at 90m (beam size 4''3 × 4''1).</figcaption></figure>

a larger map going out to 10% of the primary beam sensitivity and inspecting visually the spectra in this region. We concluded that the emission is real, but at the limit of significance. We will therefore not include this emission in our quantitative analysis. The higher-resolution image (lower panel), shows that the NE, and even more the SW, cloud consist of various smaller clouds.

Based on this distribution of the CO, we defined different regions in the galaxy, corresponding to the NE and SW cloud and the total emission (see Fig. 3). For each region, we determined the integrated spectrum which is shown in Fig. 4. The line widths in the two regions are ~20 km s⁻¹ (SW) and ~25 km s⁻¹ (NE). We then determined the velocity integrated flux of the spectra by integrating over channels with emission. The error was calculated as ΔS = σ√ΔVdV where dV is the width of a channel (1.6 km s⁻¹), ΔV is the velocity range over which the integration was carried out and σ is the rms noise level, determined in the part of the spectrum where no emission was detected. The values are measured from the taper90 map, but the agreement with the taper50 map is within ~10%. The results are listed in Table 2. We can compare the value to the total flux obtained over the same area with the IRAM 30 m telescope of 7.5 Jy km s⁻¹ (Duc et al. 2007), with an estimated error of about 20%. Thus, the interferometric observations yield about (70 ± 15)% of the flux from

<figure><img src="image_5.png" /><figcaption>Fig. 4. CO spectra (black lines), integrated over different regions (see Fig. 3 for the corresponding apertures), overlaid with the HI spectra (red dashed lines) in the same areas.</figcaption></figure>

single-dish observations, showing that at most a small fraction of smoothly distributed, diffuse CO may be resolved out.

We calculated the mass of the molecular gas from the PdBI CO fluxes as

$$M_{\text{mol}} = 1.05 \times 10^4 D_{\text{Mpc}}^2 S_{\text{CO(1-0)}} M_{\odot}, \quad (1)$$

where $D_{\text{Mpc}}^2$ is the distance in Mpc and $S_{\text{CO(1-0)}}$ is the CO(1–0) flux in Jy km s⁻¹ (see Bolatto et al. 2013). This expression is based on a conversion factor of $X_{\text{CO}} = 2 \times 10^{20} \text{ cm}^{-2}/(\text{K km s}^{-1})$ and includes a mass fraction of helium of 1.36. The molecular gas masses are listed in Table 2, together with the molecular mass surface densities, which were calculated by dividing the mass by the area over which the CO flux was integrated.
<figure><img src="image_6.png" /><figcaption>**Fig. 5.** Left panel: u-band image overlayed with the CO (red contours) and HI emission (blue contours). CO contours are at ~0.2, 0.4, 0.6 and 0.8 Jy km s⁻¹ beam⁻¹, corresponding to Σ<sub>mol</sub> ~ 2, 4, 6 and 8 M<sub>☉</sub> pc⁻². HI contours are at Σ<sub>atom</sub> ~ 2, 4, 6, and 8 M<sub>☉</sub> pc⁻². The bar to the bottom-left corner corresponds to 1 kpc. Middle panel: HI velocity field overlayed with the CO emission (contours are the same as in the left panel). The blue cross and ellipse illustrate, respectively, the centre and extent of the HI disc investigated by Lelli et al. (2015). The black circle and dashed line show, respectively, the centre and orientation of the slice used to obtain the PV diagrams. Right panel: PV diagrams obtained from the HI and CO cubes along the dashed line in the middle panel. Contours range from 3 to 15σ in steps of 3σ, where σ = 4.5 mJy beam⁻¹ for CO data (red) and σ = 0.6 mJy beam⁻¹ for HI data (black). The horizontal line corresponds to the systemic velocity of the HI disc.</figcaption></figure>

<table><caption>**Table 2.** CO(1–0) velocity integrated flux (from 1129 to 1159 km s⁻¹), S<sub>CO</sub>, molecular gas mass, mean molecular surface density, atomic gas mass, mean atomic surface density, and molecular gas mass fraction in different regions.</caption><thead><tr><th>Region</th><th>Area<br>[kpc<sup>2</sup>]</th><th>S<sub>CO</sub><br>[Jy km s<sup>-1</sup>]</th><th>M<sub>mol</sub><br>[10<sup>6</sup> M<sub>☉</sub>]</th><th>Σ<sub>mol</sub><br>[M<sub>☉</sub> pc<sup>-2</sup>]</th><th>M<sub>atom</sub><sup>b</sup><br>[10<sup>6</sup> M<sub>☉</sub>]</th><th>Σ<sub>atom</sub><br>[M<sub>☉</sub> pc<sup>-2</sup>]</th><th>M<sub>mol</sub>/M<sub>gas</sub></th></tr></thead><tbody><tr><td>NE</td><td>2.9</td><td>3.4 ± 0.2</td><td>10.3 ± 0.6</td><td>3.6 ± 0.2</td><td>26 ± 3</td><td>8.9 ± 0.9</td><td>0.28 ± 0.03</td></tr><tr><td>SW</td><td>1.7</td><td>2.0 ± 0.2</td><td>6.1 ± 0.6</td><td>3.5 ± 0.4</td><td>13 ± 1</td><td>7.9 ± 0.8</td><td>0.32 ± 0.05</td></tr><tr><td>Total<sup>a</sup></td><td>5.2</td><td>5.4 ± 0.2</td><td>16.4 ± 0.6</td><td>3.2 ± 0.1</td><td>46 ± 5</td><td>8.9 ± 0.9</td><td>0.26 ± 0.03</td></tr></tbody></table>

Notes. (a) “Total” refers to the CO-emitting area for both the molecular and the atomic gas mass, not to the total HI area of the TDG (see Fig. 5).

(b) For consistency with the molecular gas, we include in the atomic gas mass a helium fraction of 1.36.

## 3.2. Comparison of CO and HI emission

Figure 5 compares the distribution and kinematics of CO and HI emission. The left panel shows an *u*-band image overlaid with both the total CO map at ~7'' resolution (red) and the HI map at ~14'' resolution (blue). The CO cloud to the NE coincides with a strong HI peak (Σ<sub>atom</sub> ~ 8 M<sub>☉</sub> pc⁻²) and several stellar clusters. The CO cloud to the SW, instead, lies between two HI peaks; faint star clusters are present in this region. The molecular gas fraction is around 30% everywhere (see Table 2) which is in the range of what Casoli et al. (1998) found for spiral galaxies of type Sa-Sc, and much higher than their result for Sd spirals and irregulars (less than 5%).

The middle panel shows the HI velocity field (from Lelli et al. 2015) overlaid with the total CO map. Lelli et al. (2015) analysed high-resolution HI data of VCC 2062 and found that the HI emission can be described by a rotating disc model. The blue cross and ellipse in Fig. 5 illustrate, respectively, the centre and extension of the HI disc as derived by Lelli et al. (2015). Clearly, the CO emission is displaced to the SW of the kinematic centre, lying on the approaching, blue-shifted side of the HI disc. The NE half of the HI disk contains only older stars.

The right panel compares Position-Velocity (PV) diagrams derived from the HI and CO cubes (red and black contours, respectively). There is excellent agreement between HI and CO kinematics. The HI gas has a broader line width than the

CO gas (see also Fig. 4 for a direct comparison of the CO and HI spectra), which is most likely due to the lower velocity and angular resolutions of the HI data. The horizontal line indicates the HI systemic velocity: clearly the CO mainly probes the kinematics on the approaching side of the disc. The shape of the CO PV diagrams suggests a rising rotation curve that perhaps flattens in the outer parts, as it is often seen in dwarf galaxies (e.g. Swaters et al. 2009; Lelli et al. 2012a,b). We note, however, that these PV diagrams do not correspond exactly to the disc major axis (they were chosen to go through the peaks of the CO emission), hence they do not capture the full disc rotation (cf. Fig. 5 of Lelli et al. 2015). Towards the very SW, outside the ellipse showing the extension of the HI disk, the HI emission is not consistent anymore with a rotating disc; it is representative of the underlying tidal debris, showing broad and asymmetric HI line profiles.

## 3.3. Comparison of CO with the distribution of SF regions

In Fig. 6 we show an overlay of the CO emission (contours) with the 8 µm emission. The NE CO cloud coincides with considerable SF, visible in all tracers, whereas at the position of the SE cloud weaker 8 µm. SF traced by 8 µm is also present close to the emission of the tentative weak southern CO cloud, close to the edge of our field of view.
<figure><img src="image_7.png" /><figcaption>**Fig. 6.** Overlay of IRAC 8 µm data (colour) and CO contours (black contours), starting at 0.15 Jy km s⁻¹ beam⁻¹ (~3σ) and incrementing in steps of 0.1 Jy km s⁻¹ beam⁻¹. The blue dashed contours show the apertures used for the measurement of the SFR and molecular gas. The outer black line shows the Field of View of the PdBI observations.</figcaption></figure>

# 4. Spectral Energy Distribution and modelling

## 4.1. Photometry

We made use of the multiwavelength maps available for VCC 2062 and determined the Spectral Energy Distribution (SED) from the FUV to 24 µm. We used the same aperture for all bands and carried out the photometry in 2 areas, (i) an aperture encompassing the entire object visible in the optical, including an extended area with weaker emission and no signs of substantial young SF, as traced for example by $H\alpha$ or 8 µm emission (see the lower left image in Fig. 1); and (ii) an aperture encompassing the total CO emission (the same aperture as in Fig. 3). For each image, we subtracted the average sky background measured in close-by regions outside of the main aperture. For the *Spitzer* images we applied, following the IRAC and *Spitzer* handbooks aperture correction factors of 0.95, 0.97, 0.88 and 0.83 for the IRAC bands 1 to 4 and a factor of 1.12 for the MIPS 24 µm band. For the NGVS data no aperture corrections were necessary due to their high angular resolution compared to the aperture size. For the GALEX images we estimated the aperture correction from the 8 µm image which shows a similar structure. The aperture correction was derived as the ratio between the flux of the original 8 µm map to the flux from the 8 µm map convolved to the GALEX resolution. We derived values for the aperture correction of 2% for the FUV and 3% for the NUV emission.

We determined the error as the quadratic sum of 3 components: (i) the photometric error due to the noise in the image. This component was usually negligible. (ii) The error due to variations in the background level, estimated from the differences of the mean values in the various background apertures. (iii) Calibration uncertainty as listed in Table 1.

The fluxes derived are listed in Table 3. They are corrected for a Galactic extinction of $A_V = 0.11$, based on the Schlafly & Finkbeiner (2011) recalibration of the Schlegel et al. (1998) extinction values and extrapolated using the Cardelli et al. (1989) extinction law with $R_V = 3.1$.

<table><caption>**Table 3.** Fluxes for the total emission in various bands.</caption><thead><tr><th rowspan="2">Band</th><th rowspan="2">λ<br>[µm]</th><th colspan="2">Flux<br>[mJy]</th></tr><tr><th>total galaxy</th><th>CO area</th></tr></thead><tbody><tr><td>FUV (GALEX)</td><td>0.154</td><td>0.055 ± 0.005</td><td>0.039 ± 0.004</td></tr><tr><td>NUV (GALEX)</td><td>0.232</td><td>0.083 ± 0.005</td><td>0.051 ± 0.003</td></tr><tr><td>u (NGVS)</td><td>0.381</td><td>0.19 ± 0.02</td><td>0.10 ± 0.01</td></tr><tr><td>g (NGVS)</td><td>0.487</td><td>0.32 ± 0.03</td><td>0.15 ± 0.01</td></tr><tr><td>i (NGVS)</td><td>0.769</td><td>0.35 ± 0.03</td><td>0.17 ± 0.01</td></tr><tr><td>z (NGVS)</td><td>0.887</td><td>0.33 ± 0.06</td><td>0.15 ± 0.02</td></tr><tr><td>IRAC1 (Spitzer)</td><td>3.5</td><td>0.23 ± 0.03</td><td>0.14 ± 0.02</td></tr><tr><td>IRAC2 (Spitzer)</td><td>4.5</td><td>0.19 ± 0.02</td><td>0.10 ± 0.01</td></tr><tr><td>IRAC3 (Spitzer)</td><td>5.8</td><td>0.83 ± 0.35</td><td>0.59 ± 0.14</td></tr><tr><td>IRAC4 (Spitzer)</td><td>8.0</td><td>1.9 ± 0.4</td><td>1.3 ± 0.2</td></tr><tr><td>MIPS1 (Spitzer)</td><td>24</td><td>1.3 ± 0.7</td><td>1.0 ± 0.3</td></tr></tbody></table>

## 4.2. SED modelling with CIGALE

To estimate physical properties of VCC 2062, we modelled the SED with the latest release of the CIGALE code<fnref n="4" /> (version number 0.8.1, Boquien et al., in prep.). We built a grid of models, including different SF histories, stellar populations, attenuations (shape of the attenuation curve and normalisation), and emission by dust. The full grid is made of 20 966 400 models. In more detail, these components cover the following parameter space:

1. Guided by the high UV/$H\alpha$ luminosity ratio, we modelled the SF history by a double decaying exponential. The first exponential represents the long term SF of the object, starting 13 Gyr ago and with an *e*-folding time ranging from 1 Gyr to 8 Gyr in steps of 1 Gyr. The second exponential represents the latest star-forming episode having started between 50 Myr and 500 Myr ago, with an *e*-folding time from 50 Myr to 500 Myr, both in steps of 50 Myr. This second episode is assumed to have formed between 0.1% and 50% (the sampling being 0.1%, 0.5%, 1%, 5%, 10%, and afterwards increasing in steps of 5% until 50%) of the total stellar mass.

2. The stellar populations are assumed to have a constant, solar metallicity of $Z = 0.02$. This metallicity is appropriate for VCC 2062 which has $12 + \log(O/H) = 8.6$ (Duc et al. 2007), close to the Solar metallicity of $12 + \log(O/H) = 8.66$ (Asplund et al. 2005).

3. We adopt a Chabrier (2003) Initial Mass Function (IMF), which is very similar to the Kroupa IMF.

4. The stellar populations are attenuated with a power-law-modified starburst extinction law ($A(\lambda) = A(\lambda)_{SB} \times (\lambda/550 \text{ nm})^\delta$, with $-0.5 \le \delta \le 0.0$ (in steps of 0.1)). The $E(B-V)$ reddening of stars younger than 10 Myr is comprised between 0.1 mag and 0.75 mag (increasing in steps of 0.05 mag). Young stars that have not yet broken out completely from their birth clouds tend to be more attenuated than the old stellar population (e.g. Calzetti 2013). In order to take this into account, we apply a reduction factor (0.25, 0.50, or 0.75) to the reddening of old stars.

<footnote n="4">⁴ http://cigale.lam.fr</footnote>
<figure><img src="image_8.png" /><figcaption>**Fig. 7.** Observed SED of VCC 2062, together with the best fit derived with CIGALE. In the bottom panels the residuals from the comparison between model and observations are shown.</figcaption></figure>

5. The emission of dust is computed from the absorbed energy from the UV to the near-infrared through an energy balance principle, modelled using the Dale et al. (2014) template, with the $\alpha$ parameter varying between 0.5 and 4.0, in steps of 0.5.

Finally, the physical properties such as the SFR, the stellar mass, or the attenuation are estimated from the full grid of models through a Bayesian-like analysis of their respective marginalised probability distribution function.

We show the best fit for the total galaxy in Fig. 7. The most relevant best-fit parameters are listed in Table 4 (both for the total galaxy and for the CO-emitting region). The stellar emission was fitted by a combination of a burst and an underlying older component. The mass fraction in the burst (~40%) is found to be considerable but the exact value is not well constrained. The age of the burst of about 0.3 Gyr is consistent with the expected age of the merger (several hundred Myr). The SFR has been declining by a factor of about 1.4 during the last 100 Myr.

The SED of VCC 2062 has been modelled before by Boquien et al. (2010). The present analysis includes two major improvements. (i) The quality of the data set has improved substantially. Apart from a higher image quality in the optical range, the data set now includes high-quality data in the i and z-bands which were absent or very poor in Boquien et al. (2010). (ii) The modelling is done with the CIGALE code instead of PE-GASE which was used in Boquien et al. (2010). The most relevant improvement in CIGALE is that the fitting process relies on a Bayesian estimate of the marginalised probability distribution functions, allowing more reliable estimates of the physical properties and the associated uncertainties. Furthermore, the entire SED from the UV to the IR is modelled consistently now, with the energy absorbed in the UV being re-emitted in the IR by the dust. This allows us to make use of the mid-IR emission which is crucial to break the age-attenuation degeneracy of the object. The results obtained here remain broadly consistent with those from Boquien et al. (2010), but represent a considerable improvement, for example with respect to the SFR which could not be determined reliably in the previous study.

<table><caption>**Table 4.** Best-fit parameters derived with the CIGALE SED-fitting.</caption><thead><tr><th>Parameter</th><th>Total galaxy</th><th>CO area</th></tr></thead><tbody><tr><td>present SFR (10<sup>-3</sup> M<sub>☉</sub> yr<sup>-1</sup>)</td><td>3.9 ± 0.9</td><td>3.0 ± 0.4</td></tr><tr><td>past SFR<sup>a</sup> (10<sup>-3</sup> M<sub>☉</sub> yr<sup>-1</sup>)</td><td>5.4 ± 1.0</td><td>3.7 ± 0.7</td></tr><tr><td>total stellar mass (10<sup>6</sup> M<sub>☉</sub>)</td><td>7.1 ± 2.0</td><td>3.1 ± 0.9</td></tr><tr><td>age of the burst (Myr)</td><td>376 ± 99</td><td>313 ± 86</td></tr><tr><td>A<sub>V</sub> (mag)</td><td>0.24 ± 0.06</td><td>0.28 ± 0.06</td></tr><tr><td>A<sub>FUV</sub> (mag)</td><td>1.25 ± 0.17</td><td>1.31 ± 0.15</td></tr></tbody></table>

Notes. (a) SFR averaged over the past $10^8$ yr.

## 5. The SF law in VCC 2062

### 5.1. Calculation of the star formation rate

The high-resolution CO data allows us to study the SF law separately for the NE cloud and SW cloud, as well as for the region encompassing the entire molecular gas emission. Hence, we are probing SF on a ~kpc scale (the linear sizes of the NE and SW regions are 2.5 and 1.6 kpc, respectively). We calculated the SFR using different tracers which allows us to obtain a complete picture of the SF history. Whereas $H\alpha$ is emitted from the most massive, ionizing stars and traces the very recent SFR (~10 Myr), the UV radiation is emitted mostly by stars of several solar masses and probes the SFR over the past 100–200 Myr. Both emissions need to be extinction-corrected, which can introduce a considerable uncertainty. The emissions by dust at 8 µm and 24 µm have the advantage of being, due to their long wavelengths, practically extinction-free SF tracers, but they rely on the presence of dust and might therefore miss the fraction of SF which is not attenuated. The combinations of stellar and dust emission (here we use 8 µm, 24 µm and $H\alpha$/UV) are expected to be the most reliable tracers as they are sensitive to both dust-free and dust-enshrouded regions with no need to apply an extinction correction (see Kennicutt & Evans 2012).

We carried out aperture photometry on the FUV, $H\alpha$, 8 µm and 24 µm images using the aperture as following the CO emission (total emission, NE and SW cloud, see Fig. 3). In addition, we derived the flux for the highest-resolution SFR tracers, $H\alpha$ and 8 µm using smaller apertures centred on peaks of the 8 µm emission (see Fig. 6). In order to take the different angular resolutions of the data into account we performed a Gaussian convolution on the $H\alpha$ and 8 µm map to the resolution of the taper90 CO data (4′/2). The resolution of the GALEX FUV map is comparable to that of the taper90 CO. On the other hand, the resolution of the 24 µm is slightly worse. We ignore this effect because it is expected to be small compared to the flux uncertainty and because the 24 µm emission is not our main SF tracer. In this analysis we give more weight to the combined 8 µm and $H\alpha$ emission which has a higher resolution and higher signal-to-noise.

The stellar contribution to the 8 µm was found to be less than 0.5% in the CIGALE modelling, and therefore we assume that the 8 µm emission is entirely emitted by dust. We corrected the UV emission for Galactic foreground extinction (see Sect. 3.5). We furthermore applied a correction for the internal extinction based on the values derived in the SED modelling with CIGALE (Table 4). The total extinction correction of the UV flux was significant (a factor ~4). The extinction correction of the $H\alpha$ flux was very small (0.07 mag, or a factor of 1.06), derived from the $H\alpha/H\beta$ ratio (Duc et al. 2007).
We used the prescriptions in Tables 1 and 2 of Kennicutt & Evans (2012) to derive SFRs, both from monochromatic and mixed (stellar+dust dust emission) tracers, except for the calculation of the SFR from the 24 µm emission where we used the relation derived by Calzetti et al. (2007) from resolved observations ($SFR = 1.27 \times 10^{-38} L_{24\mu m}^{0.885} (erg s^{-1})$). In addition we used the relation from Zhu et al. (2008) to derive the SFR from the 8 µm emission ($SFR = 1.2 \times 10^{-43} L_{8\mu m} (erg s^{-1})$). All SFRs were calculated for a Kroupa IMF (Kroupa 2001) which is very similar to the Chabrier IMF used in the CIGALE modelling.

The resulting values for the SFR, together with the SFR surface densities, $\Sigma_{SFR}$, are listed in Table 5. The uncertainty in the SFRs is only partly due to the error in the fluxes from which they are calculated, but more by the intrinsic uncertainty in the calibration of the SFR tracers which can be up to a factor of 2 (Leroy et al. 2012). The dust derived and combined tracers give similar results in all regions. The SFR derived from the $H\alpha$ emission yields a SFR which is a factor ~2 lower while the UV emission tends to give a higher SFR by a factor of ~2 (both compared to dust derived and combined tracers). The largest difference is thus between the SFR derived from FUV and from $H\alpha$ (factor 2–5). This result could be due to the sensitivity of both tracers to extinction which makes them less robust than the combined tracers. The higher SFR derived from the UV could also be the result of the decreasing SFR after a single burst of SF and the short life-time of the $H\alpha$ compared to the UV emitting stars. Interestingly, such an effect has also been found by Lee et al. (2009) for a sample of ~300 dwarf galaxies that showed, in contrast to spiral galaxies, a systematically lower SFR from $H\alpha$ than from UV (all SFR tracers having been corrected for extinction).

## 5.2. Comparison to star formation laws

Figure 8 shows the comparison of $\Sigma_{SFR}$ to the surface density of the CO-derived molecular gas, as the phase that is more closely related to SF, for different regions in VCC 2062 in a classical Kennicutt-Schmidt (KS) plot. We show the values derived for the different regions (NE, SW and entire CO-emitting area) and different tracers from Table 5. Furthermore we show the values for the small apertures centred on the SF peaks in the NE region. We also include the present and past SFR surface density derived from the SED fitting with CIGALE (Table 4). We compare the data from VCC 2062 to those of a sample of spatially resolved observations of nearby galaxies from HERACLES (Bigiel et al. 2011)$^5$. From these data, as well as from the earlier studies by Bigiel et al. (2008) and Leroy et al. (2008), a linear relation between $\Sigma_{H2}$ and $\Sigma_{SFR}$ has been found for angular scales between 180 pc and 1.7 kpc. Bigiel et al. (2011) compared the HERACLES data to an extensive data set of galaxies from the literature and found a consistent trend, albeit with an increased scatter (about 0.5 dex). Their linear relationship implies a constant gas depletion time of ~2.35 Gyr which can be interpreted as a constant SFE per molecular cloud.

In Fig. 9 (left) we show a similar relation, but now comparing $\Sigma_{SFR}$ to the surface density of the total (molecular and HI) gas. We include, for comparison, data for the galaxy sample from Kennicutt (1998), spanning from spiral to starburst galaxies, and the corresponding fit to those data which is a power-law in the form $\Sigma_{SFR} \propto \Sigma_{gas}^{1.4}$.

As a third SF law we test the relation proposed by Krumholz et al. (2012; Fig. 9, middle). They derived a good relation between $\Sigma_{SFR}$ and $\Sigma_{gas}/\tau_{ff}$, holding from molecular cloud scales to starburst galaxies, where $\tau_{ff}$ is the local free-fall time of the gas. This quantity can be calculated, assuming that the molecular gas is distributed in GMCs, as

$$ \tau_{ff} = \frac{\pi^{1/4}}{\sqrt{8}} \left[ \frac{\sigma}{G \Sigma_{GMC}^3 \Sigma_{gas}} \right]^{1/4}, \quad (2) $$

where G is the gravitational constant, $\sigma$ the gas velocity dispersion, $\Sigma_{GMC}$ the surface density of a typical molecular cloud, adopted, following Krumholz et al. (2012), as $85 M_{\odot} pc^{-2}$, and $\Sigma_{gas}$ the average gas surface density in the region where the stars form. We adopt for the molecular gas the same velocity dispersion as for the atomic gas ($\sigma = 7 \text{ km s}^{-1}$, Lelli et al. 2015). We note, however, that this model should be applied with caution to VCC 2062 where not only gravitational but also tidal forces might be important.

The values of $\Sigma_{SFR}$ of VCC 2062 lie below all these three relations. The difference is particularly large for the SFR derived from the hybrid SF indicators, and largest for the SW cloud (more than a factor of 10). The difference for the SFRs derived from the extinction-corrected UV emission and with CIGALE are less pronounced. They are on the low side, just outside the scatter, of what is expected from the spiral galaxy sample. The values of both $\Sigma_{SFR}$ and $\Sigma_{mol}$ depend on the size of the aperture and increase for smaller apertures which are centred on peaks of the SF region. However, they still lie well below the three relations even for the smaller apertures.

As a final test, we looked into the relation between $\Sigma_{SFR}$ and $\Sigma_{gas}/\tau_{orb}$ (Elmegreen 1997; Silk 1997). Kennicutt (1998) found that this prescription adjusted the data as well as just with $\Sigma_{gas}$. Moreover, starburst galaxies at high redshifts seem to deviate from the standard KS relation but adhere to its kinematical version with orbital times (Daddi et al. 2010; Genzel et al. 2010). This relation implies that per rotation period about 10% of the available gas is converted into stars. The physical reason for this relation is still open and includes processes such as spiral density waves or, in a slightly modified model, cloud-cloud collisions (Tan 2000) or cloud collapse due to a large-scale Toomre instability (Krumholz et al. 2012). Intriguingly, a similar relation between $\Sigma_{SFR}$ and $\Sigma_{gas}/\tau_{orb}$ also holds for dwarf galaxies, which lack a well-defined spiral pattern and are probably forming stars in a HI-dominated regime (Lelli et al. 2014). There are, however, also observations that do not strongly support this prescription. Leroy et al. (2008) compared the orbital timescale to the radial variation of the SFE and concluded that $\tau_{orb}$ alone cannot explain SF, and Krumholz et al. (2012) showed that a relation between $\Sigma_{SFR}$ and $\Sigma_{gas}/\tau_{orb}$ is not able to explain the process of SF from very small (molecular clouds) to large (starburst) scales.

Due to the lack of DM, VCC 2062 has a long orbital period of, derived from the HI, $1.2 \times 10^9$ yr (Lelli et al. 2015). Together with the mean gas depletion time of ~1–2 × 10$^{10}$ yr (derived from the mixed tracers, see Table 4) we derive a gas consumption time per revolution of 6–12% in the range of the value of 10% found by Kennicutt (1998) In Fig. 9 (right) we compare the relation derived with this value for VCC 2062 to that of the sample from Kennicutt (1998). Indeed, VCC 2062 follows this relation well, with a very good agreement for the NE region and the total emission and an offset towards low values only for the SE region. The similarity of the SFE per revolution in VCC 2062 and spiral/starburst galaxies could indicate that galaxy-wide processes related to the rotation are responsible

<footnote>$^5$ The SFR and gas masses for this sample and the other samples used for comparison, are adapted to our choice of the IMF, CO-to-H$_2$ conversion factor and helium fraction.</footnote>
<table><caption>**Table 5.** SFR parameters for the different regions.</caption><thead><tr><th>Band</th><th>Flux<sup>a</sup><br>[mJy]<sup>d</sup><br>[10<sup>-15</sup> erg cm<sup>-2</sup> s<sup>-1</sup>]<sup>d</sup></th><th>Luminosity<sup>a</sup><br>[10<sup>38</sup> erg s<sup>-1</sup>]</th><th>SFR<sup>b</sup><br>[10<sup>-4</sup> M<sub>☉</sub> yr<sup>-1</sup>]</th><th>τ<sub>dep</sub><sup>c</sup><br>[10<sup>10</sup> yr]</th><th>Σ<sub>SFR</sub><sup>b</sup><br>[10<sup>-4</sup> M<sub>☉</sub> yr<sup>-1</sup> kpc<sup>-2</sup>]</th></tr></thead><tbody><tr><td colspan="6"><strong>Total emission</strong></td></tr><tr><td>FUV</td><td>0.039 ± 0.004</td><td>265.4</td><td>39.1</td><td>0.42</td><td>7.56</td></tr><tr><td>Hα</td><td>4.24 ± 0.42</td><td>1.46</td><td>7.8</td><td>2.1</td><td>1.52</td></tr><tr><td>8 μm</td><td>1.25 ± 0.18</td><td>161.33</td><td>19.4</td><td>0.8</td><td>3.74</td></tr><tr><td>8 μm+Hα</td><td>—</td><td>—</td><td>17.8</td><td>0.9</td><td>3.44</td></tr><tr><td>24 μm</td><td>1.00 ± 0.30</td><td>43.19</td><td>15.2</td><td>1.1</td><td>2.95</td></tr><tr><td>24 μm+FUV</td><td>—</td><td>—</td><td>19.4</td><td>0.8</td><td>3.77</td></tr><tr><td>24 μm+Hα</td><td>—</td><td>—</td><td>12.5</td><td>1.3</td><td>2.43</td></tr><tr><td colspan="6"><strong>NE cloud</strong></td></tr><tr><td>FUV</td><td>0.030 ± 0.003</td><td>205.2</td><td>30.2</td><td>0.54</td><td>10.47</td></tr><tr><td>Hα</td><td>3.76 ± 0.38</td><td>1.22</td><td>6.6</td><td>1.6</td><td>2.27</td></tr><tr><td>8 μm</td><td>0.92 ± 0.12</td><td>118.67</td><td>14.2</td><td>0.7</td><td>4.94</td></tr><tr><td>8 μm+Hα</td><td>—</td><td>—</td><td>13.9</td><td>0.7</td><td>4.82</td></tr><tr><td>24 μm</td><td>0.87 ± 0.18</td><td>37.33</td><td>13.3</td><td>0.8</td><td>4.54</td></tr><tr><td>24 μm+FUV</td><td>—</td><td>—</td><td>15.7</td><td>1.0</td><td>5.33</td></tr><tr><td colspan="6"><strong>SW cloud</strong></td></tr><tr><td>FUV</td><td>0.008 ± 0.001</td><td>51.7</td><td>7.6</td><td>2.2</td><td>4.43</td></tr><tr><td>Hα</td><td>0.60 ± 0.06</td><td>0.19</td><td>1.0</td><td>5.9</td><td>0.60</td></tr><tr><td>8 μm</td><td>0.26 ± 0.05</td><td>33.26</td><td>4.0</td><td>1.5</td><td>2.32</td></tr><tr><td>8 μm+Hα</td><td>—</td><td>—</td><td>3.1</td><td>2.0</td><td>1.79</td></tr></tbody></table>

**Notes.** (a) The fluxes and luminosities are corrected for Galactic foreground emission as explained in Sect. 3.5. (b) The SFRs derived from the UV flux takes into account both the Galactic foreground extinction and an internal extinction derived from the stellar population fit (see Table 3 and Sect. 3.6). (c) Molecular gas depletion timescale, calculated as the ratio between the SFR from column 4 and the molecular gas mass from Table 1. (d) The unit for most fluxes entries is mJy, expect for Hα which is given in 10<sup>-15</sup> erg cm<sup>-2</sup> s<sup>-1</sup>. (e) We did not detect any significant emission at 24 μm in the SW region.

for the collapse of molecular clouds. If this were the reason we would expect a similar result for TDGs in general. For the TDG in Arp 158 (Boquien et al. 2011), the two TDGs in Stephan's Quintet (Lisenfeld et al. 2004) and a small sample of TDGs detected in CO (Braine et al. 2001), τ<sub>dep</sub> could be estimated and was found – contrary to VCC 2062 – to be similar to that of spiral galaxies (1–3 × 10<sup>9</sup> yr). These observations are mostly based on single pointings with the IRAM 30 m telescope which do not resolve the structure of the TDGs and therefore do not allow us to apply kinematical models to derive τ<sub>orb</sub>. Thus, the analysis of the available data of other TDGs does not allow to draw any firm conclusions with respect to the role played by τ<sub>orb</sub> in the SF process.

## 5.3. The specific star formation rate

We used the present SFR and the stellar mass derived from the stellar population CIGALE fitting to calculate the specific SFR (sSFR), as sSFR = SFR/M*, yielding sSFR = 5.5 × 10<sup>-10</sup> yr<sup>-1</sup>. This value lies in the range typical for low-mass spiral galaxies with stellar masses of 10<sup>8</sup>–10<sup>9</sup> M<sub>☉</sub> (see Kennicutt & Evans 2012, for a summary). Applying the relation from Schiminovich et al. (2007; log(sSFR) = -0.36 log(M*) – 6.4) we would expect a somewhat higher sSFR for the low-mass VCC 2062 (M* = 7 × 10<sup>6</sup> M<sub>☉</sub>), of the order of 10<sup>-9</sup> yr<sup>-1</sup>. The most likely reason for the somewhat lower value is that VCC 2062 is a recycled galaxy so that part of its stars might come from the parent galaxy and have not formed in situ. Figure 2 supports this conclusion since it clearly shows a bridge of old stars from NGC 4695 to VCC 2062. We can test this by

<figure><img src="image_9.png" /></figure>

**Fig. 8.** SFR surface density as a function of the molecular gas surface density. The values are calculated for the NE cloud, the SW cloud, the total area where CO is detected (see Fig. 3 for the apertures), as well as for smaller apertures centred on the peaks of the 8 μm emission in the NE cloud (see Fig. 6 for the apertures, labelled here NL, NN and NS for the largest aperture, northern and southern apertures, respectively). The data of VCC 2062 compared to the results of a spatially resolved analysis of HERACLES galaxies (Bigiel et al. 2011). The black dots are their data points obtained at a 1 kpc angular resolution, the solid black line shows their best-fit relation obtained and the dashed line its standard deviation.
<figure><img src="image_10.png" /></figure>

**Fig. 9.** SFR surface density as a function of the total (H₂+HI+He) gas surface density (**left panel**), gas surface density per free-fall time (**middle panel**) and gas surface density per orbital timescale (**right panel**). The values for VCC 2062 (red, magenta and blue) are labelled as in Fig. 8. The SFR has been calculated with different tracers (see Sect. 5 and Table 5). **Left:** the values for VCC 2062 are compared to the sample of Kennicutt (1998). **Middle:** the surface density of the SFR is compared to the molecular surface density per free-fall time, following Krumholz et al. (2012). The values for VCC 2062 are compared to the sample of Kennicutt (1998). The red dashed line gives the relation for a 1% efficiency, the value that Krumholz et al. (2012) find to describe the data well. **Right:** the surface density of the SFR is compared to the molecular surface density per orbital timescale. A value of $\tau_{\text{orb}} = 1.2 \times 10^9$ yr (Lelli et al. 2015) is adopted for VCC 2062. The comparison sample is from Kennicutt (1998). The red dashed line gives the relation for a 10% efficiency, the value that Kennicutt (1998) find as their average value.

deriving the sSFR only in the part of the galaxy where recent SF takes place, assuming that all the stars here have formed in VCC 2062. When we use the CIGALE value for the SFR and $M_*$ for the CO-emitting area and derive $\text{sSFR} = 9 \times 10^{-10} \text{ yr}^{-1}$, close to the expected value.

# 6. Discussion

## 6.1. VCC 2062 as an old TDG

Duc et al. (2007) studied VCC 2062 in detail and concluded that it is most likely an old TDG. In this study we confirm this view. Two important new pieces of evidence reinforce the past conclusion. (i) A kinematical analysis by Lelli et al. (2015) shows that there is no evidence for DM in VCC 2062, as predicted for this class of objects. (ii) The deep NGVS image reveals a bridge between NGC 4694 and VCC 2062 (see Fig. 2), clearly showing the connection between these objects. Besides, the new deep image shows that the putative parent galaxy exhibits many tidal disturbances consistent with the hypothesis that it is the result from a major gas-rich merger, i.e. the type of collisions able to form TDGs.

The large, multiwavelength data set available for VCC 2062 has allowed detailed analysis of the present and past SF, making VCC 2062 the TDG with the best-studied SED. Previous, similar studies of TDGs and intergalactic SF regions (Boquien et al. 2007, 2009, 2010), had to base their SED modelling on a more incomplete wavelength range which limited the conclusions, for example about the old stellar population. Our analysis shows that the SFR has been declining in the past with a burst that took place about ~300 Myr ago and included a considerable fraction of the mass of the object. This timescale is shorter than the typical merger timescale of ~1 Gyr (Bournaud 2010), consistent with the picture that the SF has taken place in the TDG.

The mass fraction of stars formed in the burst (~40%) is higher than typical values in spiral and dwarf galaxies (see Gil de Paz et al. 2003, finding that the burst strengths is <1% in Blue Compact Dwarf Galaxies) and typical of what is found

in TDGs for which in some cases no old stellar population is found at all (Boquien et al. 2009, 2010). An open question that remains is which fraction of the old stellar population is actually associated with the gravitationally bound object, VCC 2062, and which part belongs to the tidal tail, visible in Fig. 2. About half of the stellar mass derived for the entire object is situated in the CO-emitting region with young SF. Most likely, at least this fraction of the stellar mass belongs to VCC 2062. However, in order to definitively conclude this, deep spectroscopical observations determining the kinematical association of the old stars with VCC 2062 or the tail would be necessary.

## 6.2. Comparison to other TDGs

In Fig. 10 we show the KS-relation for a small sample of TDGs taken from the literature (see Table 6), together with the data for VCC 2062. Most of the literature data have been obtained with single dish telescopes (IRAM 30 m) and have therefore a poor angular resolution, corresponding to linear scales up to 12.2 kpc (see Table 6), much larger than the size of the SF regions. This has two consequences. (i) The surface densities are unrealistically low because the molecular gas mass and SFR are averaged over a large area. (ii) There is some uncertainty as to where on the KS-relation the objects would fall for smaller apertures centered on the SF regions.

The fact that almost all TDGs follow the standard KS-relation indicates that SF in TDGs seems to proceed in the same way as in spiral galaxies in spite of the very different local conditions (DM content, presence of spiral density waves and tidal forces) in both types of objects. The noticeable exception is VCC 2062 which lies below the standard KS-relation.

## 6.3. Why is the SFE low in VCC 2062?

The SFR surface density in VCC 2062 is below what is expected from its molecular gas surface density, both when comparing it to spiral galaxies or other TDGs. The difference is particularly large for the SW region which has only weak SF but a
<figure><img src="image_11.png" /><figcaption>**Fig. 10.** Molecular Kennicutt-Schmidt (KS) relation of a small sample of TDGs for which data for molecular gas and the SFR is available in the literature (see Table 6 for the values and references). Most observations are carried out with a single-dish telescope (IRAM 30 m telescope) except for two objects in Stephan's Quintet (SQ) which are marked with a square symbol. We also include the values for VCC 2062 from IRAM 30 m data (black short line), both for the entire galaxy (lower end of the line) and for a single pointing centred on the NE region (upper end of the line). The Bigiel et al. (2011) relation for spiral galaxies and the PdBI values for VCC 2062 (in red, magenta and blue) are shown.</figcaption></figure>

considerable amount of molecular gas. The difference is larger for SFRs based on dust and $H\alpha$ than for those based on UV or CIGALE modelling. Furthermore, the difference decreases for smaller apertures which are centred on the peaks of SF visible in 8 µm within the NE region, but is still there. Thus, even though the exact value of the SFE varies with the choice of SF tracer and with the angular resolution, we find the consistent result that the SFE is low in VCC 2062 compared to other TDGs and spiral galaxies.

The molecular gas surface density in VCC 2062 is very low, among the lowest probed in similar studies (e.g. Bigiel et al. 2008, 2011; Schruba et al. 2011). SF in low gas surface densities has been studied in the outskirts of galaxies (Schruba et al. 2011) or in LSB galaxies (Boissier et al. 2008; Wyder et al. 2009) and very low values of SFE(gas) = SFR/M\_gas have been found. However, in these regions molecular gas formation is not very efficient and the molecular gas fraction is low. Possibly, the SFE based on the (undetected) molecular gas would have been normal. This is indeed what has been found in the outskirts of galaxies by stacking the CO spectra Schruba et al. (2011). These results are consistent with the picture that at low surface brightnesses the formation of molecular gas is inefficient, but when it is present, it forms stars with the same SFE as in the inner disks of spirals. The situation in the LSB galaxy VCC 2062 is very different from the objects described above. Here, the molecular gas fraction is considerable ($M_{mol}/M_{HI} \approx 0.3$). The question is why this molecular gas is forming stars at a very low efficiency.

VCC 2062 is not the only object with abundant molecular gas but little SF. Similar situations have been observed in other unusual objects, for example in some regions of the TDG candidate J1023+1952 in the system Arp 94 (Lisenfeld et al. 2008),

<table><caption>**Table 6.** Data for the molecular gas and SFR for a sample of TDGs.</caption><thead><tr><th>Name</th><th>Dist<br>[Mpc]</th><th>FWHM<br>["/kpc]</th><th>Area<br>[kpc<sup>2</sup>]</th><th>M<sub>mol</sub><br>[10<sup>7</sup> M<sub>☉</sub>]</th><th>SFR<br>[10<sup>-2</sup> M<sub>☉</sub> yr<sup>-1</sup>]</th><th>Ref.</th></tr></thead><tbody><tr><td>Arp158</td><td>62.1</td><td>22/6.6</td><td>49.3</td><td>8.5</td><td>5.0</td><td>(1)</td></tr><tr><td>Arp105S</td><td>115.0</td><td>22/12.2</td><td>169.9</td><td>19.8</td><td>8.1</td><td>(2)</td></tr><tr><td>NGC4676N</td><td>90.0</td><td>22/9.6</td><td>201.5</td><td>10.3</td><td>8.1</td><td>(2)</td></tr><tr><td>NGC7252W</td><td>64.0</td><td>11/3.3</td><td>12.6</td><td>1.3</td><td>0.5</td><td>(2)</td></tr><tr><td>SQB</td><td>85.0</td><td>22/10.0</td><td>112.2</td><td>48.3</td><td>32.2</td><td>(2,3)</td></tr><tr><td>SQB</td><td>85.0</td><td>4/1.6</td><td>21.2</td><td>34.0</td><td>30.0</td><td>(4)</td></tr><tr><td>SQtip</td><td>85.0</td><td>4/1.6</td><td>5.0</td><td>11.0</td><td>5.0</td><td>(4)</td></tr><tr><td>J1032+1952</td><td>20.4</td><td>22/2.2</td><td>6.0</td><td>10.5</td><td>2.4</td><td>(5)</td></tr><tr><td>Arp245N</td><td>31.0</td><td>22/3.3</td><td>27.0</td><td>19.0</td><td>9.0</td><td>(6,7)</td></tr><tr><td>VCC 2062 (NE)</td><td>17</td><td>22/1.8</td><td>7</td><td>2.3</td><td>0.2</td><td>(8,9)</td></tr><tr><td>VCC 2062 (total)</td><td>17</td><td>22/1.8</td><td>2.7</td><td>1.4</td><td>0.2</td><td>(8,9)</td></tr></tbody></table>

**Notes.** All data are adapted to include He in the molecular gas mass and to a Kroupa IMF. The SFR is mostly derived from $H\alpha$ except for Arp 158 where it is derived from FUV and 24 µm. The area denotes the area over which the $M_{mol}$ and SFR have been determined which can be larger than the resolution of the observation.

**References.** (1) Boquien et al. (2011); (2) Braine et al. (2001; Table 2) and reference therein; (3) Lisenfeld et al. (2002a); (4) Lisenfeld et al. (2004); (5) Lisenfeld et al. (2008); (6) Braine et al. (2000); (7) Duc et al. (2000); (8) Duc et al. (2007) (for the CO from IRAM 30 m); (9) this paper (for the SFR).

the intergalactic bridge in Stephan's Quintet (Lisenfeld et al. 2002a; Guillard et al. 2012), the face-on colliding Taffy galaxies (Braine et al. 2003, 2004), some galaxies in Hickson Compact Groups (HCG; Alatalo et al. 2015) or in the gas in tails stripped from galaxies in clusters (Jáchym et al. 2014; Verdugo et al. 2015). The reason for the lack of SF in spite of the presence of abundant, CO-traced molecular gas is not completely clear, and might be different in each case. A possible reason is the lack of a dense molecular gas phase, as in the bridge of the Taffy galaxies. Braine et al. (2003) showed for this system that molecular gas reformed quickly after the collision, but the dense molecular cores were destroyed. In galaxies in HCGs, Alatalo et al. (2015) argued that shock-injected turbulence perturbed the molecular gas and decreased the SFE.

The situation in VCC 2062 is probably different from the above examples. It is most likely a self-gravitating object, similar to other TDGs in which, in general, the SFE seems normal (see Sect. 5.2). However, the much lower surface brightness of VCC 2062, both with respect to the gas and to the stars, is a major difference between VCC 2062 and other studied TDGs. The stellar surface density ($0.6 M_{☉} pc^{-2}$ within the CO-emitting area) is considerably lower than $\Sigma_{gas}$ which may lead to a flaring in the gas disk, similar to what is seen in the outer disks of spirals and irregular galaxies (Elmegreen & Hunter 2015), causing a decrease in the volume density of the gas. An additional effect of the low surface density of newly formed stars is that their combined radiation pressure is less efficient in dispersing the molecular gas. Thus, we might simply be seeing the remaining molecular gas, left-over after the formation of stars. Due to the low stellar surface brightness the interstellar radiation field and thus the gas temperature are most likely low. Shetty et al. (2011) showed that there is only a weak dependence of $X_{CO}$ on the gas temperature, $T$, ($X_{CO} \propto T^{-0.5}$ for $T \sim 20-100$ K). Apart from being weak, the direction of this dependence means that we might slightly underestimate the molecular gas mass, and thus overestimate the SFE, i.e. making the difference with respect to spiral galaxies even larger.

The kinematic information of the gas allows us to apply the stability criterium of Toomre (1964) and derive the critical gas
surface density for SF as

$$ \Sigma_{\text{crit,gas}} = \frac{\alpha\sigma\kappa}{\pi G}, \qquad (3) $$

where α is a constant which we adopt, following Martin & Kennicutt (2001), as α = 0.69 and κ is the epicyclic frequency. We derived critical densities of 2 and 4 M☉ pc⁻² for the SW and NE regions, albeit with a high uncertainty (factor 2–3), mostly because of the uncertainty in the rotation velocity which is a factor of 2 (see Table 7 in Lelli et al. 2015). However, even considering this uncertainty, the observed gas surface densities (between 11 and 13 M☉ pc⁻², see Table 2) seem to be above the estimated critical value so that the gas is expected to be able to form stars.

Finally, the fact that VCC 2062 is a small object where SF is intermittent might play a role when comparing its SF law to that of larger spiral galaxies where local variations average out more easily. In fact, the analysis of the HI distribution and kinematics (Lelli et al. 2015) has shown that the SF regions are distributed in a very asymmetric way in VCC 2062 (see Fig. 5). The young SF regions all lie on one side of the kinematical centre, whereas the old stars, traced by optical emission, are found also on the other side and extend to the tidal tail connecting VCC 2062 to the parent galaxy. Temporal variations in the SF history could have two consequences. (i) The calibration of the SF tracers is different from that in spiral galaxies. Indeed, Leroy et al. (2012) has shown that SF tracers are not reliable and do not give very consistent results among themselves on kpc scales and for values of Σ<sub>SFR</sub> ≤ 10⁻² M☉ yr⁻¹ kpc⁻¹. (ii) Our observations might be sensitive to short temporal variations in the ratio between SFR tracers and molecular gas mass which would average out in larger spiral galaxies. Such an effect is expected to be particularly relevant on small angular scales as in the small and faint region SE where the SFE is indeed particularly low.

In summary, there are a number of reasons why the SFE in VCC 2062 is low. We cannot firmly conclude which are the most relevant ones, and very likely, several of them play a role. In any case, it is very likely that the low surface brightness of the object (both in stars and gas) plays an important role in lowering the gas density, decreasing the stellar radiation feedback and increasing the uncertainties in the standard SFR tracers.

## 7. Summary and conclusions

We presented new CO(1–0) data obtained with the Plateau de Bure Interferometer of VCC 2062, a nearby TDG at the outskirts of the Virgo Cluster. These data have allowed us to study the molecular gas distribution and kinematics. Using a large set of complementary data we modelled the UV-to-IR SED and derived the SFR from different tracers. Combining the SFR with the CO data, we studied the SF law in this object. TDGs have two important properties that make this analysis particularly interesting: (i) In contrast to classical dwarf galaxies, their metallicity is higher (typically of the order of 0.5–0.3 of the Milky Way value) and therefore CO is a good tracer of the molecular gas; and (ii) their DM content is very low and so we are able to study SF in this extreme, DM-free environment. The main conclusions are summarised as follows.

- The CO emission is distributed in two main regions, called NE and SW. The NE region coincides with the peak of the atomic gas and with SF tracers, whereas the SW region lies in between two HI peaks and has little associated SF.

- A comparison of the atomic and molecular gas showed that the atomic gas is more extended than the CO and young SF regions. CO is only found on one side of the kinematical centre of the galaxy. The HI and CO kinematics agree well in the regions where their emissions coincide.

- New, deep optical observations of this system with the NGVS revealed a stellar bridge between the parent galaxy NGC 4695 and VCC 2062. This, together with the negligible dark matter content found from HI kinematical modelling (Lelli et al. 2015), gives the final proof that VCC 2062 is a TDG.

- We modelled the UV-to-IR SED with CIGALE and found that the SFR has noticeably declined in the recent past (a factor of 1.3–1.4 between the present SFR and the SFR averaged over the past 10⁸ yr).

- We calculated the SFR from various tracers (UV, Hα, 8, and 24 µm and combinations of them). In general the different tracers gave compatible results with the exception of the UV which gave a factor ~2–4 higher SFR. A declining SFR or a paucity of massive stars are possible reasons. The SFR surface density derived from the dust emission and Hα was lower than those derived by the SED modelling from CIGALE by a factor of ~2–3.

- The molecular gas depletion time (=M<sub>mol</sub>/SFR), derived at different angular resolutions between 0.3 and ~1.5 kpc, of about 1–2 × 10¹⁰ Gyr, derived from Hα and dust tracers, is long compared to the median value found by Bigiel et al. (2011; τ<sub>dep</sub> = 2.35 Gyr, for different samples of galaxies). The discrepancy is particularly large for the SW region (gas depletion time of ~6 × 10¹⁰ yr). Similar discrepancies were found when comparing VCC 2062 to other SF laws (Kennicutt 1998; Krumholz et al. 2012).

- We compare the SFE of VCC 2062 to a small sample of other TDGs, most of them with data for the molecular gas at a poorer angular resolution. We find that TDGs in general follow the same KS-relation as spiral galaxies and that VCC 2062 is the only exception.

- We discussed various possible reasons for this long molecular gas depletion time. The difference is not due to an inefficient formation of the molecular gas since abundant molecular gas is present. The low surface brightness of VCC 2062 most likely plays an important role in changing the physical conditions compared to more massive objects (decreased mid-plane pressure, low stellar radiation field). Temporal effects due to intermittent SF and uncertainties in the calibration of the SF tracer might also play a role.

- Together with the orbital timescale τ<sub>orb</sub> derived from the HI analysis (1.2 × 10⁹ yr, Lelli et al. 2015), we derived a gas consumption per orbit of 6–12%, in the range of the value of 10% derived for spiral and starburst galaxies in spite of the lack of DM in VCC 2062. High-resolution data for other TDGs are necessary in order to find out whether this result holds for TDGs in general which would indicate an important role of τ<sub>orb</sub> in the SF process.

*Acknowledgements.* We would like to warmly thank our support astronomer at Plateau de Bure, A. Castro-Carrizo, for dedicated help during the data reduction, and F. Bigiel for making his data available to us. We appreciate the referee’s very useful comments which helped derive firmer conclusions from the data. This project made use of data obtained as part of the CFHT NGVS Large Programme. The data were processed by Jean-Charles Cuillandre and Stephen Gwyn under the supervision of Laura Ferrarese and Patrick Côté. They are warmly thanked. U.L. acknowledges support by the research projects AYA2011-24728 and AYA2014-53506-P financed by the Spanish Ministerio de Economía y Competitividad and by FEDER (Fondo Europeo de
Desarrollo Regional) and the Junta de Andalucía (Spain) grants FQM108. E.B. acknowledges support from the UK's Science and Technology Facilities Council (grant numbers ST/J001333/1, ST/M001008/1). This work is based on observations carried out under project number ue1e-2010 with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the use of the HyperLeda database (http://leda.univ-lyon1.fr).

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**Appendix A: Channel maps**

Figure A.1 shows the channel maps of the taper50 data cube. Emission is visible in the velocity range between 1129 and 1159 km s⁻¹, distributed in various clouds and showing a velocity gradient along the NE–SW direction.

<figure><img src="image_12.png" /><figcaption>**Fig. A.1.** Channel maps of the emission tapered to 50 m baseline length. The beam (size 7′′7 × 6′′3) is shown at the lower left corner of each image. The cross indicates the central position of the observations.</figcaption></figure>