Context : V1180 Cas is a young variable that has shown strong photometric fluctuations ( \Delta I \sim 6 mag ) in the recent past , which have been attributed to events of enhanced accretion .
The source has entered a new high-brightness state in September 2013 , which we have previously analysed through optical and near-infrared spectroscopy .

Aims : To investigate the current active phase of V1180 Cas , we performed observations with the Chandra satellite aimed at studying the X-ray emission from the object and its connection to accretion episodes .

Methods : Chandra observations were performed in early August 2014 .
Complementary JHK photometry and J -band spectroscopy were taken at our Campo Imperatore facility to relate the X-ray and near-infrared emission from the target .

Results : We observe a peak of X-ray emission at the nominal position of V1180 Cas and estimate that the confidence level of the detection is about 3 \sigma .
The observed signal corresponds to an X-ray luminosity L _ { X } ( 0.5-7 kev ) in the range 0.8 \div 2.2 \times 10 ^ { 30 } erg s ^ { -1 } .
Based on the relatively short duration of the dim states in the light curve and on stellar luminosity considerations , we explored the possibility that the brightness minima of V1180 Cas are driven by extinction variations .
From the analysis of the spectral energy distribution of the high state we infer a stellar luminosity of 0.8-0.9 L _ { \odot } and find that the derived L _ { X } is comparable to the average X-ray luminosity values observed in T Tauri objects .
Moreover , the X-ray luminosity appears to be lower than the X-ray emission levels around 5 \times 10 ^ { 30 } \div 1 \times 10 ^ { 31 } erg s ^ { -1 } detected at outbursts in similar low-mass objects .

Conclusions : Our analysis suggests that at least part of the photometric fluctuations of V1180 Cas might be extinction effects rather than the result of accretion excess emission .
However , because the source displays spectral features indicative of active accretion , we speculate that its photometric variations might be the result of a combination of accretion-induced and extinction-driven effects , as suggested for other young variables , such as V1184 Tau and V2492 Cyg .