M85 optical transient 2006-1 (M85 OT 2006-1) is the most luminous member of
the small family of V838 Mon-like objects, whose nature is still a mystery.
This event took place in the Virgo cluster of galaxies and peaked at an
absolute magnitude of I~-13. Here we present Hubble Space Telescope images of
M85 OT 2006-1 and its environment, taken before and after the eruption, along
with a spectrum of the host galaxy at the transient location. We find that the
progenitor of M85 OT 2006-1 was not associated with any star forming region.
The g and z-band absolute magnitudes of the progenitor were fainter than about
-4 and -6 mag, respectively. Therefore, we can set a lower limit of ~50 Myr on
the age of the youngest stars at the location of the progenitor that
corresponds to a mass of <7 solar mass. Previously published line indices
suggest that M85 has a mean stellar age of 1.6+/-0.3 Gyr. If this mean age is
representative of the progenitor of M85 OT 2006-1, then we can further
constrain its mass to be less than 2 solar mass. We compare the energetics and
mass limit derived for the M85 OT 2006-1 progenitor with those expected from a
simple model of violent stellar mergers. Combined with further modeling, these
new clues may ultimately reveal the true nature of these puzzling events.Comment: 4 pages, accepted to Ap

A. Jordan

A. Rau

Brown N. J.

D. Magee

E. O. Ofek

E. W. Peng

J. P. Blakeslee

L. D. Bradley

L. Ferrarese

P. Cote

R. Bouwens

S. B. Cenko

S. Mei

S. R. Kulkarni

T. Puzia

English

arXiv

International audienceM85 Optical Transient 2006-1 (M85 OT 2006-1) is the most luminous member of the small family of V838 Mon-like objects, whose nature is still a mystery. This event took place in the Virgo Cluster of galaxies and peaked at an absolute magnitude of MI~-13. Here we present Hubble Space Telescope images of M85 OT 2006-1 and its environment, taken before and after the eruption, along with a spectrum of the host galaxy at the transient location. We find that the progenitor of M85 OT 2006-1 was not associated with any star-forming region. The g- and z-band absolute magnitudes of the progenitor were fainter than about -4 and -6 mag, respectively. Therefore, we can set a lower limit of ~50 Myr on the age of the youngest stars at the location of the progenitor that corresponds to a mass o

Ofek, E. O.

Kulkarni, S. R.

Rau, A.

Cenko, S. Bradley

Peng, Eric W.

Blakeslee, John P.

Côté, Patrick

Ferrarese, Laura

Jordán, Andrés

Mei, Simona

Puzia, Thomas H.

Bradley, L. D.

Magee, D.

Bouwens, R.

Hal-Diderot

The Environment of M85 Optical Transient 2006-1: Constraints on the Progenitor Age and Mass

HAL: Hyper Article en Ligne

HAL-OBSPM

Cenko, S. B.

Peng, E. W.

Blakeslee, John

C\uf4t\ue9, P.

Jord\ue1n, A.

Mei, S.

Puzia, Thomas

NRC Publications Archive

HAL-INSU

M85 Optical Transient 2006-1 (M85 OT 2006-1) is the most luminous member of the small family of V838 Mon-like objects, whose nature is still a mystery. This event took place in the Virgo Cluster of galaxies and peaked at an absolute magnitude of MI ≈ -13. Here we present Hubble Space Telescope images of M85 OT 2006-1 and its environment, taken before and after the eruption, along with a spectrum of the host galaxy at the transient location. We find that the progenitor of M85 OT 2006-1 was not associated with any star-forming region. The g- and z-band absolute magnitudes of the progenitor were fainter than about –4 and –6 mag, respectively. Therefore, we can set a lower limit of ~50 Myr on the age of the youngest stars at the location of the progenitor that corresponds to a mass of <7 M⊙. Previously published line indices suggest that M85 has a mean stellar age of 1.6 ± 0.3 Gyr. If this mean age is representative of the progenitor of M85 OT 2006-1, then we can further constrain its mass to be less than 2 M⊙. We compare the energetics and mass limit derived for the M85 OT 2006-1 progenitor with those expected from a simple model of violent stellar mergers. Combined with further modeling, these new clues may ultimately reveal the true nature of these puzzling events

Blakeslee, J. P.

Côté, P.

Ferrarese, L.

Jordán, A.

Meinardi, S.

Puzia, T.

Caltech Authors - Main

THE ENVIRONMENT OF M85 OPTICAL TRANSIENT 2006-1:
CONSTRAINTS ON THE PROGENITOR AGE AND MASS
E. O. Ofek,1 S. R. Kulkarni,1 A. Rau,1 S. B. Cenko,1 E. W. Peng,2 J. P. Blakeslee,3 P. Coˆte´,2 L. Ferrarese,2
A. Jorda´n,4 S. Mei,5 T. Puzia,2 L. D. Bradley,6 D. Magee,7 and R. Bouwens7
Received 2007 July 12; accepted 2007 October 9
ABSTRACT
M85 Optical Transient 2006-1 (M85 OT 2006-1) is the most luminous member of the small family of V838
MonYlike objects, whose nature is still a mystery. This event took place in the Virgo Cluster of galaxies and peaked
at an absolute magnitude ofMI  13. Here we presentHubble Space Telescope images of M85 OT 2006-1 and its
environment, taken before and after the eruption, along with a spectrum of the host galaxy at the transient location.
We find that the progenitor of M85 OT 2006-1 was not associated with any star-forming region. The g- and z-band
absolute magnitudes of the progenitor were fainter than about4 and6 mag, respectively. Therefore, we can set a
lower limit of50 Myr on the age of the youngest stars at the location of the progenitor that corresponds to a mass
of<7M. Previously published line indices suggest that M85 has a mean stellar age of 1:6  0:3 Gyr. If this mean
age is representative of the progenitor of M85 OT 2006-1, then we can further constrain its mass to be less than 2M.
We compare the energetics and mass limit derived for the M85 OT 2006-1 progenitor with those expected from a
simple model of violent stellar mergers. Combined with further modeling, these new clues may ultimately reveal the
true nature of these puzzling events.
Subject headings: stars: individual (M85 OT 2006-1, V838 Mon, M31 RV, V4332 Sgr)
1. INTRODUCTION
M85 optical transient 2006-1 (M85OT 2006-1 [=J122523.82+
181056.2]) was discovered on 2006 January 6 by the Lick Ob-
servatory supernova search team (Filippenko et al. 20018) as a
faint, V  19:3 mag transient in the galaxy M85 (NGC 4382),
which is at a distance of 17.8 Mpc (Mei et al. 2007). Subsequent
spectroscopy, as well as visible light and infrared ( IR) pho-
tometry, presented in Kulkarni et al. (2007), showed that M85
OT 2006-1 has a recession velocity of 880  130 km s1, and is
therefore associated with M85. Moreover, we have shown that
the temporal and spectral properties of this object are unlike those
of supernovae, novae, or luminous blue variables.
M85OT 2006-1 peaked at absolute I-bandmagnitude of about
13. The light curve settled into a60 day plateau, followed by
a decrease in bolometric luminosity during which the blackbody
emission peak shifted toward near-IR wavelengths. The early
spectrum of M85 OT 2006-1, obtained 6 weeks after discovery,
resembles that of a4600K blackbody, with H andH narrow
emission lines (FWHM  350 km s1), along with several other
unidentified emission lines.
Spitzer SpaceTelescope IRobservations obtained about 6months
after the discovery revealed a1000K blackbody spectral energy
distribution (Rau et al. 2007).
The spectral and temporal properties of this object resemble
those ofM31-RV (discovered byRich et al. 1989; see, e.g.,Mould
et al. 1990; Bryan & Royer 1992), V838 Mon (discovered by
Brown 2002; see, e.g., Kimeswenger et al. 2002; Bond et al.
2003; Corradi & Munari 2007), and possibly the less studied
object V4332 Sgr (Martini et al. 1999). However, the M85 tran-
sient is the most luminous member of the V838 Mon class. The
favored model for this emerging class of V838MonYlike objects
(also known as luminous red novae9) is that they are the result
of stellar mergers (e.g., Soker & Tylenda 2006). However, other
models have been suggested to explain these objects (e.g., Retter
& Marom 2003; Lawlor 2005). The nature of these events, with
their energetics lying between the realms of supernovae and novae,
remains uncertain.
In this paper we present Hubble Space Telescope (HST ) Ad-
vanced Camera for Surveys (ACS)/Wide Field Camera (WFC)
and Near Infrared Camera and Multi-Object Spectrometer
(NICMOS) observations, as well as Palomar 5 m spectroscopy,
of the environment of M85 OT 2006-1. The observations are
used to characterize the environment of the transient and to set
a limit on the mass of the progenitor.
2. OBSERVATIONS
M85was observed usingHSTACS in 2003 as part of theHST
ACSVirgo Cluster Survey (Coˆte´ et al. 2004). Subsequently, the
transient was observed serendipitously with ACS/WFC and
NICMOS/NIC2 in 2006 (GO-10515) as a follow-up study to
Peng et al. (2006). The ACS observations on 2006were obtained
18 days after the discovery of the transient. The log of observa-
tions, the measured magnitude of the M85 transient, or the3 
upper limit at the OT location, as derived from the HST images
taken on 2003 and 2006, are listed in Table 1. The HST images
of the galaxy and the transient environment are presented in
Figures 1 and 2.
1 Division of Physics, Mathematics and Astronomy, California Institute of
Technology, Pasadena, CA 91125.
2 Herzberg Institute of Astrophysics, Dominion Astrophysical Observatory,
Victoria, BC, Canada V9E 2E7.
3 Department of Physics andAstronomy,Washington StateUniversity, Pullman,
WA.
4 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748,
Garching, Germany.
5 GEPI, Observatoire de Paris, Section de Meudon, Meudon Cedex, France.
6 Department of Physics and Astronomy, The Johns Hopkins University,
Baltimore, MD 21218.
7 Department of Astronomy and Astrophysics, University of California, Santa
Cruz, CA 95064.
8 See http://astro.berkeley.edu /~bait / kait.html. 9 This term was introduced by Kulkarni et al. 2007.
447
The Astrophysical Journal, 674:447Y450, 2008 February 10
# 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A.
On 2007 January 20, after the M85 OT 2006-1 faded away,
we obtained a spectrum at the location of M85 OT 2006-1. The
spectrum (Fig. 3) consist of 4 ; 300 s exposures with the double
beam spectrograph mounted on the Palomar 5 m telescope. We
used the 600 lines mm1 grating blazed at 95008 in the red arm.
The 200 slit was centered on the nucleus of M85, at a position an-
gle of 185

. The position angle was chosen such that the location
of the transient will be included in the slit. On 2005 June 25,M85
was observed by Spitzerwith theMultiband Imaging Photometer
forSpitzer (MIPS). The 70m image,with exposure time of 670 s,
is shown in Figure 4.
3. RESULTS
V838MonYlike objects are found in both young regions (e.g.,
V838 Mon; AfYar & Bond 2007) and old stellar populations
(e.g.,M31RV; Bond& Siegel 2006).M85OT 2006-1 took place
in an early-type galaxy. Therefore, as we explain below, it can be
used to set an upper limit on the minimal progenitor mass that
can produce V838 MonYlike eruptions.
From the two-dimensional spectrum, shown in Figure 3, we
can set an upper limit on the flux of the H emission at the lo-
cation of M85 OT 2006-1 of <6 ; 1014 ergs cm2 s1, at the
3.5  level (equivalent to luminosity of 1:6 ; 1039 ergs s1). This
corresponds to a star formation rate smaller than about 102M yr1
(Kennicutt 1998) in a radius of100 pc around the transient lo-
cation. For comparison, theH luminosity of the Orion nebula is
about1041 ergs s1 (Haffner et al. 2003, assuming a distance of
392 pc; Jeffries 2007). Therefore, our observations rule out the
presence of a prominent star-forming region in this location.More-
over, based on the far-IR flux in the region of the transient, ob-
tained from the Spitzer MIPS 70 m image shown in Figure 4,
we can set an upper limit on the star formation rate in this region
to be less than 105 M yr1 (Kennicutt 1998).
The absence of H ii regions inM85 rule out the possibility that
the progenitor had a delay (from birth to outburst) of <10 Myr
(corresponds tok40M), which is the typical lifetime of H ii re-
gions (e.g., Mayya 1995).
An independent limit on the age and mass of the progenitor
can be inferred from the absence of stars brighter than z-band ab-
solute magnitudeMz ¼ 6:2 in the transient environment. From
the Lejeune & Schaerer (2001) stellar tracks, we find that stars
older than 50 Myr (and therefore, more massive than 7 M)
do not reach z-band absolute magnitudes brighter than Mz ¼
6:2 mag (at the red supergiant stage). We note that the z-band
stellar track magnitudes were obtained by interpolation of the I
and J bands. Therefore, we can set a lower limit on the age of the
most massive stars in the transient environment to be k50 Myr,
which corresponds to mass <7M (assuming solar metallicity).
Otherwise, we were likely to detect individual stars in this re-
gion. We note that we can limit the extinction in the transient
location to Ai < 0:8mag, based on the OT Balmer lines ratio, as-
suming case-B recombination (Kulkarni et al. 2007).
Ferrarese et al. (2006) reported possible faint wisps and patches
of dust in M85. Moreover, Schweizer & Seitzer (1992) reported
TABLE 1
Photometry and Limiting Magnitude
Limiting Magnitudeb
Date
Exposure
(s) Band Magnitudea Apparent Absolute
2003 Feb 1....... 750 F475W(g) . . . >26.9 >4.5
2003 Feb 1....... 1120 F850LP(z) . . . >25.1 >6.2
2006 Jan 24...... 2204 F475W(g) 20.57
2006 Jan 24...... 2224 F814W(i) 18.62 >25.3 >6.0
2006 Feb 28..... 500 F160W(H ) 17.82 >21.2 >10.1
a Vega-based magnitude corrected for infinite aperture (Sirianni et al. 2005).
Errors in photometry are about 0.02 mag for the ACS observations, and 0.05 mag
for the NICMOS observations. The NICMOS magnitude is calibrated using
2MASS stars in the field of view.
b Vega-based limiting magnitude as estimated by adding artificial point sources
to the images in the neighborhood of the transient and inspection of the images for
the added sources. The absolute magnitudes are calculated assuming a distance
of 17.8 Mpc to M85 (Mei et al. 2007) and Galactic extinction of EBV ¼ 0:031
(Schlegel et al. 1998; Cardelli et al. 1989). Note, however, that distance estimates
to M85 range between 14 Mpc (Ciardullo et al. 2002) to 18.6 Mpc (Blakeslee
et al. 2001).
Fig. 1.—Left: HSTACS F814W-band image of the galaxy M85, obtained on 2006 January 24 (18 days after the discovery). The transient, which is well detected, is
marked by a circle. Right:HSTACS F475W-band image of M85 after subtraction of the best fit Sersic model (using GalFit; Peng et al. 2002). The subtracted model pa-
rameters are as follow: effective radius 38900; Sersic index 3.0; axis ratio (b/a) 0.765; position angle 29.3; diskiness 0.064. A different set of structural parameters is
obtained when analyzing the azimuthally averaged profile (Ferrarese et al. 2006). We note that the rough galaxy subtracted image allows us to show the lack of dust and
structure in the neighborhood of the transient. Note that the gray-scale level stretch in the left panel is about 5.2 times larger than in the right panel. Thewhite band in the im-
ages is due to the gap between the ACS CCDs. The slit of the Palomar 5 m telescope spectrum (Fig. 3) passes through the transient location and the center of the galaxy.
OFEK ET AL.448 Vol. 674
that M85 is somewhat bluer than typical S0 galaxies and there-
fore possibly younger. This claim is supported by Terlevich &
Forbes (2002), who estimated the age and metallicity based on
line indices. They have found a mean luminosity-weighted age of
1:6  0:3 Gyr and metallicity of ½Fe/H ¼ 0:44 and ½Mg/Fe ¼
0:08.We note that the actualmean age is probably higher than that
indicated by line indices given that younger populations have
higher weight than old population. If the mean age is representa-
tive of the progenitor of M85 OT 2006-1, then we can set a lower
limit of about 1 Gyr on the age of M85 OT 2006-1 progenitor(s).
This further suggests that the mass of the progenitor/s is prob-
ably below 2 M (the lifetime of solar metallicity >2 M stars
is <1 Gyr; Lejeune & Schaerer 2001). This limit is based on the
mean stellar age of this galaxy. However, stars younger than 1Gyr
may be present in this galaxy in relatively small numbers.
4. DISCUSSION
Although several models exist for V838 MonYlike objects
(e.g., Soker & Tylenda 2003; Lawlor 2005), in the absence of
detailed simulations, the nature of these objects remain elusive.
A clue to their origin can be derived from their environment, lu-
minosity function, and rate. Given that only a small number of
these objects are known, and they were found serendipitously in
various searches, the luminosity function and rate are not well
constrained. However, the fact that at least two events were ob-
served in our Galaxy (i.e., V838Mon and V4332 Sgr) in the last
Fig. 2.—Zoom-in on the environment of M85 OT 2006-1 HSTACS and NICMOS/NIC2 images. The circle, with radius of 100, marks the position of the transient.
Note that the F475Wþ F814W is a sum of the F475W and the F814W images.
Fig. 3.—Two-dimensional spectrum of M85 and the transient environment
(+3000 offset from the galaxy center along the slit), obtained about 1 year after the
transient discovery, covering the H wavelength region (ellipse). No H emis-
sion is seen in the vicinity of the transient. The spectrum is shown before sky
subtraction.
Fig. 4.—SpizterMIPS 70 m image of M85. The plus sign marks the visible-
light center of the galaxy, while the circle marks the position of the transient.
ENVIRONMENT OF M85 OPTICAL TRANSIENT 2006-1 449No. 1, 2008
13 years suggests that they have a higher rate than SNe. We
can set a lower limit on their rate, of 0.019 yr1 L1MW, at the 95%
confidence level, where LMW is the Milky Way luminosity.
Now we discuss the implications of our observations for a
specific model for V838 MonYlike objects. Soker & Tylenda
(2006) presented a model for violent stellar mergers in which,
prior to the merger, the spins and orbital frequencies of the bi-
nary star are losing synchronization due to the Darwin instability
(e.g., Eggleton & Kiseleva-Eggleton 2001). They found that for
a given primary mass, the maximal energy production obtained
for a binary mass ratio of 1/50, is 2:5 ; 103GM21 /R1, where
G is the gravitational constant, and M1 and R1 are the mass and
radius of the primary star. Given the upper limit on the progenitor
mass, based on the mean stellar age in M85,<2M, and assum-
ing a main-sequence mass-radius relation, R / M 0:7, the maxi-
mum available energy in their model is short by a factor of three
in the total energy production, as compared to the radiated energy
of M85 OT 2006-1 in the first 2 months, 8 ; 1046 ergs (assum-
ing a distance of 17.8 Mpc toM85; Mei et al. 2007). Moreover, it
is expected that a large fraction of the energy will go into lifting
the outer region of the star rather than radiated away. Further-
more, if the primary is an evolved star, then its radius will be
larger than the radius of a main-sequence star with the samemass,
and the extracted energy will be even smaller. This suggests that
either more detailed modeling of violent stellar mergers is re-
quired, or that this event is not the result of a violent stellar merger.
Another possible solution is that the mass of the progenitor is
somewhat larger. A larger progenitor mass will still be consistent
with our upper limit of 7 M, which is based on the absence of
stars brighter than I  6mag. For example, according to Soker
& Tylenda (2006) model, a 7M progenitor can yield 4 times
more energy than a 2 M progenitor and may explain the dis-
crepancy. We note, however, that other kinds of instabilities can
lead to stellar mergers (e.g., in triple systems) and that the above
comparison is valid only for the specific case discussed by Soker
& Tylenda (2006).
Existing hydrodynamical simulations of the common enve-
lope phase in stellar mergers (and also star + neutron star merg-
ers) predict that the total dissipated energy is of the order of
that observed in V838 Mon and M85 OT 2006-1 (e.g., Taam &
Bodenheimer 1989; Terman et al. 1995; Terman & Taam 1996).
Moreover, simulations of the common envelope phase predicts
that most of the envelope will be ejected in the equatorial plane
(e.g., Taam & Ricker 2006). Indeed, in Rau et al. (2007) we re-
ported evidence suggesting that the expansion of M85OT 2006-1
is asymmetric. However, more detailed hydrodynamical simula-
tions of the vast parameter space available for stellar mergers
are needed in order to understand these processes and to test if
V838 MonYlike objects are indeed the results of stellar mergers.
To summarize, we show that, in contrast to V838 Mon, but
similarly to M31 RV, M85 OT 2006-1 was probably produced
by members of an old stellar population (>1 Gyr), and that its
progenitor/s mass was probablyP2M. These constraints narrow
down the allowed venue of stellar models for the nature of this
event.
This work is supported in part by grants fromNSF andNASA.
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OFEK ET AL.450


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