The CoRoT ground-based complementary archive

The CoRoT ground-basedcomplementary archive

The CoRoT ground-basedcomplementary archive

Monica Rainer, Ennio PorettiM. Rosa Panzera, Angelo Mistò

INAF OABrera

M. Rainer acknowledges support from the SPACEINN grant entitled ”Exploitation of the HARPS-ESO spectra collected in the CoRoT ground based

activities”

Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

The CoRoT ground-based

complementary archiveA large ground-based high-

resolution spectroscopic campaign

has been performed from the

launch of the CoRoT satellite (27th

December 2006) up to January

2013.

The spectroscopy complements the

photometric CoRoT observations of

asteroseismic targets.

Ground-based spectroscopyP.I. Ennio Poretti

[email protected] ESO-

LaSilla


LaSillaP.I. Philippe Mathias

[email protected] OHPP.I. Pedro Amado

[email protected] Calar

AltoP.I. Katrien Uytterhoeven

FIES@NOT ORMP.I. Conny Aerts

HERMES@MERCATOR ORM


LaSillaP.I. Karen Pollard

HERCULES@1m Mt. John

Obs.


Main studies


Most of the spectra are already been used for dedicated studies.

This large dataset of variable objects can still be exploited either

for more detailed single studies or for statistical and comparative

analysis.

HARPS spectra

For now we will build our archive using only the HARPS

spectra, that are homogenoeusly reduced and

normalised.

7150 spectra

269 objects


The ESO archive

The HARPS spectra are already stored in the ESO

archive, where both the raw data and the spectra

reduced by the HARPS pipeline at the telescope can be

found.

We have reduced the spectra with a different method,

using a semi-automated pipeline developed at the

Brera Observatory.


Reduced HARPS spectra

Automated pipeline result

Our pipeline result


Normalised HARPS spectra

All the HARPS spectra have been normalised in an

automated way. The normalisation procedure has

some problems with the first orders, but it is averall

quite good.


Physical parameters

The already normalised spectra are very useful in

the determination of the stellar physical

parameters.

HD 50870Mantegazza et al., 2012, A&A 542, 24


Format of the spectra

5-columns ASCII files with wavelength,

reduced flux, normalised flux, signal-to-noise

error and number of the echelle order.

2-columns ASCII files with wavelength and

normalised flux.


The SPACEINN archive

Other than the reduced spectra, the goal of our

SPACEINN archive is to provide many additional

information, concerning both the targets and the

single spectra.

The objects will be categorised by the variability

class and, if possible, information about the time

series will be given.


Mean line profiles

The mean line profile of each spectrum will be computed and

uploaded in the archive. The profiles are obtained using the

LSD technique (Donati et al., 1997, MNRAS 291, 658) on a

sub-region of the normalised, non-merged spectra.


Mean line profiles

The mean line profile fo each spectrum will be computed and

uploaded in the archive. The profiles are obtained using the

LSD technique (Donati et al., 1997, MNRAS 291, 658) on a

sub-region of the normalised, non-merged spectra.


Mean line profiles

The high signal-to-noise

ratio of the mean line

profiles enables a more

sensitive study of the line

profile variations.

HR 6139


Pulsating binary systems

Creevey et al., 2009, A&A 507 901


Multiple systems

HD 170200


Variable classes

In the SPACEINN archive the stars will be

characterized by their variable class, in order to

enable statistical analysis of objects of the same

kinds.

Some information on the most peculiar

characteristic of the variable will be given.


Be stars

In the case of the Be stars, we would like to give some

information on the strength and symmetry of the H-alpha

emission.

HD 49330 Floquet et al., 2009, A&A 506, 103


δ Scuti stars


δ Scuti stars


Activity index

It is possible to compute an activity index from the

CaII H and K lines to be stored in the SPACEINN

archive.


The files

For each observed spectrum, the archive will contain

three different FITS files, with VO-compliant headers:

a 5-field table with wavelength, reduced flux,

normalised flux, signal-to-noise ratio and echelle

order;

a 2-field table with wavelength and normalised

flux, where the echelle orders have been merged;

a 2-field table (velocity and normalised flux) storing

the mean line profile computed using the LSD

software.Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

Information on the object

Looking for a variable class will return a list of objects

with their physical parameters, such as:

effective temperature, logg, metallicity;

binarity flag (none, SB1, SB2)

spectral type

information on the pulsational content of the time

series, if more than a few spectra are present in the

archive.


Information on the spectrum

Looking for an object will return a list of spectra with

some characterizing information such as:

date of the observation, HARPS mode;

signal-to-noise ratio at a predefined wavelength;

radial velocity and vsini;

activity index, emission index (Be), tbd.


Other capabilities

The user should be able to plot the spectra and the

mean line profiles and zoom them.

We would like to offer the possibility of either

plotting or downloading radial velocity curves and

other relevant quantities.


Study example

We hope that this archive

will be useful for

comparative or statistical

studies.

The spectra are already

being used in this way, but

the web interface will allow

much easier access.


Milestones

T0 + 12

Availability of the reduced spectra with full indicators

T0 + 18

Availability of simultaneous photometric and

spectroscopic curves

T0 + 24

Definition of the query interface

T0 + 30

Opening to the community


Conclusion: what we have

The reduced data and large part of the mean line

profiles.

An estimate of the physical paramenters for many

objects, but we would like to complete the work on the

whole database.

Reliable HARPS radial velocities for the objects

observed in HAM mode (R = 115,000), but we will need to

compute them for the ones observed in the EGGS mode

(R = 80,000).

Binarity flags for most of the objects.


Conclusion: work to do

Complete the previous work.

Calibrate a reliable activity index.

Determine ad hoc information on the time series in

order to give an hint on the pulsational content (i.e.,

the standard deviation of the mean line profiles from

the average mean line profile).

Defining the archive interface and the kind of output

given.


Documents

The CoRoT ground-based complementary archive