We present the results of new observations of the enigmatic radio source B1144+352 with the WSRT at 1.4 GHz .
This source is hosted by an m _ { r } = 14.3 \pm 0.1 galaxy at a redshift of z = 0.063 \pm 0.002 and is one of the lowest redshift Gigahertz Peaked Spectrum ( GPS ) sources known .
It has been known to show radio structure on pc-scale in the radio core and on 20 - 60 kpc-scale in two jet-like radio structures .
The WENSS and NVSS surveys have now revealed faint extended radio structures on an even much larger scale .
We have investigated these large-scale radio components with new 1.4-GHz WSRT observations .
Our radio data indicate that the eastern radio structure has a leading hotspot and we conclude that this structure is a radio lobe originating in the galaxy hosting the GPS source .
The western radio structure contains two separate radio sources which are superposed on the sky .
The first is a low-power radio source , hosted by a m _ { R } = 15.3 \pm 0.5 galaxy at a similar redshift ( z = 0.065 \pm 0.001 ) to the GPS host galaxy ; the second is an extended radio lobe , which we believe is associated with the GPS host galaxy and which contains an elongated tail .
The total projected linear size of the extended radio structure associated with B1144+352 is \sim 1.2 Mpc .
The core of B1144+353 is a known variable radio source : its flux density at 1.4 GHz has increased continuously between 1974 and 1994 .
We have measured the flux density of the core in our WSRT observations ( epoch 1997.7 ) and find a value of 541 \pm 10 mJy .
This implies that its flux density has decreased by \sim 70 mJy between 1994 and 1997 .
Further , we have retrieved unpublished archival ROSAT HRI data of B1144+352 .
The source has been detected and appears to be slightly extended in X-rays .
We find a luminosity of ( 1.26 \pm 0.15 ) \times 10 ^ { 43 } erg s ^ { -1 } between 0.1 and 2.4 keV , assuming that the X-ray emission is due to an AGN with a powerlaw spectrum with photon index 1.8 , or ( 0.95 \pm 0.11 ) \times 10 ^ { 43 } erg s ^ { -1 } if it is due to thermal bremsstrahlung at T = 10 ^ { 7 } K. The detection of the X-ray source suggests that the intrinsic H i column density can not be much larger than a few times 10 ^ { 21 } cm ^ { -2 } .
The non-detection of an extended X-ray halo in a radius of 250 kpc around the host galaxy limits the X-ray luminosity of an intra-cluster gas component within this radius to \la 2.3 \times 10 ^ { 42 } erg s ^ { -1 } ( 1 \sigma upper limit ) .
This is below the luminosity of an X-ray luminous cluster and is more comparable to that of poor groups of galaxies .
Also the optical data show no evidence for a rich cluster around the host galaxy .
B1144+352 is the second GPS galaxy known to be associated with a Mpc-sized radio source , the other being B1245+676 .
We argue that the observed structure in both these GPS radio sources must be the result of an interrupted central jet-activity , and that as such they may well be the progenitors of sources belonging to the class of double-double radio galaxy .